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ADS astronomy entries on 2022-09-14
author:"Sauval, A. Jacques"
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Title: The elemental composition of the Sun. III. The heavy elements
Cu to Th
Authors: Grevesse, Nicolas; Scott, Pat; Asplund, Martin; Sauval,
A. Jacques
2015A&A...573A..27G Altcode: 2014arXiv1405.0288G
We re-evaluate the abundances of the elements in the Sun from copper
(Z = 29) to thorium (Z = 90). Our results are mostly based on
neutral and singly-ionised lines in the solar spectrum. We use the
latest 3D hydrodynamic solar model atmosphere, and in a few cases
also correct for departures from local thermodynamic equilibrium
(LTE) using non-LTE (NLTE) calculations performed in 1D. In order
to minimise statistical and systematic uncertainties, we make
stringent line selections, employ the highest-quality observational
data and carefully assess oscillator strengths, hyperfine constants
and isotopic separations available in the literature, for every line
included in our analysis. Our results are typically in good agreement
with the abundances in the most pristine meteorites, but there are
some interesting exceptions. This analysis constitutes both a full
exposition and a slight update of the relevant parts of the preliminary
results we presented in Asplund et al. (2009, ARA&A, 47, 481),
including full line lists and details of all input data that we have
employed. <P />Tables 1-3 are available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201424111/olm">http://www.aanda.org</A>
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Title: The elemental composition of the Sun. II. The iron group
elements Sc to Ni
Authors: Scott, Pat; Asplund, Martin; Grevesse, Nicolas; Bergemann,
Maria; Sauval, A. Jacques
2015A&A...573A..26S Altcode: 2014arXiv1405.0287S
We redetermine the abundances of all iron group nuclei in the Sun,
based on neutral and singly-ionised lines of Sc, Ti, V, Mn, Fe, Co and
Ni in the solar spectrum. We employ a realistic 3D hydrodynamic model
solar atmosphere, corrections for departures from local thermodynamic
equilibrium (NLTE), stringent line selection procedures and high
quality observational data. We have scoured the literature for
the best quality oscillator strengths, hyperfine constants and
isotopic separations available for our chosen lines. We find log
ɛ<SUB>Sc</SUB> = 3.16 ± 0.04, log ɛ<SUB>Ti</SUB> = 4.93 ± 0.04,
log ɛ<SUB>V</SUB> = 3.89 ± 0.08, log ɛ<SUB>Cr</SUB> = 5.62 ± 0.04,
log ɛ<SUB>Mn</SUB> = 5.42 ± 0.04, log ɛ<SUB>Fe</SUB> = 7.47 ± 0.04,
log ɛ<SUB>Co</SUB> = 4.93 ± 0.05 and log ɛ<SUB>Ni</SUB> = 6.20 ±
0.04. Our uncertainties factor in both statistical and systematic errors
(the latter estimated for possible errors in the model atmospheres and
NLTE line formation). The new abundances are generally in good agreement
with the CI meteoritic abundances but with some notable exceptions. This
analysis constitutes both a full exposition and a slight update of the
preliminary results we presented in Asplund et al. (2009, ARA&A,
47, 481), including full line lists and details of all input data
we employed. <P />Tables 1-3 are available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201424110/olm">http://www.aanda.org</A>
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Title: The elemental composition of the Sun. I. The intermediate
mass elements Na to Ca
Authors: Scott, Pat; Grevesse, Nicolas; Asplund, Martin; Sauval,
A. Jacques; Lind, Karin; Takeda, Yoichi; Collet, Remo; Trampedach,
Regner; Hayek, Wolfgang
2015A&A...573A..25S Altcode: 2014arXiv1405.0279S
The chemical composition of the Sun is an essential piece of reference
data for astronomy, cosmology, astroparticle, space and geo-physics:
elemental abundances of essentially all astronomical objects are
referenced to the solar composition, and basically every process
involving the Sun depends on its composition. This article, dealing
with the intermediate-mass elements Na to Ca, is the first in a
series describing the comprehensive re-determination of the solar
composition. In this series we severely scrutinise all ingredients
of the analysis across all elements, to obtain the most accurate,
homogeneous and reliable results possible. We employ a highly
realistic 3D hydrodynamic model of the solar photosphere, which has
successfully passed an arsenal of observational diagnostics. For
comparison, and to quantify remaining systematic errors, we repeat
the analysis using three different 1D hydrostatic model atmospheres
(marcs, miss and Holweger & Müller 1974, Sol. Phys., 39, 19) and
a horizontally and temporally-averaged version of the 3D model (⟨ 3D
⟩). We account for departures from local thermodynamic equilibrium
(LTE) wherever possible. We have scoured the literature for the best
possible input data, carefully assessing transition probabilities,
hyperfine splitting, partition functions and other data for inclusion
in the analysis. We have put the lines we use through a very stringent
quality check in terms of their observed profiles and atomic data, and
discarded all that we suspect to be blended. Our final recommended
3D+NLTE abundances are: log ɛ<SUB>Na</SUB> = 6.21 ± 0.04, log
ɛ<SUB>Mg</SUB> = 7.59 ± 0.04, log ɛ<SUB>Al</SUB> = 6.43 ± 0.04,
log ɛ<SUB>Si</SUB> = 7.51 ± 0.03, log ɛ<SUB>P</SUB> = 5.41 ± 0.03,
log ɛ<SUB>S</SUB> = 7.13 ± 0.03, log ɛ<SUB>K</SUB> = 5.04 ± 0.05
and log ɛ<SUB>Ca</SUB> = 6.32 ± 0.03. The uncertainties include both
statistical and systematic errors. Our results are systematically
smaller than most previous ones with the 1D semi-empirical
Holweger & Müller model, whereas the ⟨ 3D ⟩ model returns
abundances very similar to the full 3D calculations. This analysis
provides a complete description and a slight update of the results
presented in Asplund et al. (2009, ARA&A, 47, 481) for Na to
Ca, and includes full details of all lines and input data used. <P
/>Tables 1-4 and Appendix A are available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201424109/olm">http://www.aanda.org</A>
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Title: “Old” versus “New” Solar Chemical Composition
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P.
2013ASPC..479..481G Altcode:
We follow the evolution since 1989 of element abundance determinations
in the solar photosphere. We describe how the largely used high
metallicity mixtures (Z = 0.02 to 0.017) of Anders & Grevesse
(1989), Grevesse & Noels (1993) and Grevesse & Sauval (1998)
have been obtained and explain why these mixtures should not be used
anymore. They are to be replaced by the more recent mixture of Asplund
et al. (2009) which results from the first comprehensive and homogeneous
analysis for many decades. We describe the main characteristics of this
work and discuss some impacts of this low Z (Z = 0.0134) mixture. We
also comment on another recent analysis by Caffau et al. (2011) that
leads to somewhat larger metal abundances.
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Title: The New Solar Chemical Composition — from Z = 0.02 to Z
= 0.013
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P.
2012ASPC..462...41G Altcode:
We review the current status of our knowledge of the chemical
composition of the sun and present a redetermination of the solar
abundances of all available elements. These new results have recently
been published by Asplund et al. (2009). The basic ingredients of
this work, the main results and their implications are discussed. We
show why the abundances of the main contributors to the metallicity
have decreased and why the old high solar metallicity, Z ∼ 0.02,
is definitely obsolete and should not be used anymore. We also show
why other recent analyzes of the solar composition report solar
metallicities somewhat larger than the one we recommend.
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Title: The chemical composition of the sun
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P.
2011CaJPh..89..327G Altcode:
No abstract at ADS
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Title: The New Solar Composition and the Solar Metallicity
Authors: Grevesse, Nicolas; Asplund, Martin; Sauval, A. Jacques;
Scott, Pat
2011sswh.book...51G Altcode:
No abstract at ADS
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Title: The chemical composition of the Sun
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P.
2010Ap&SS.328..179G Altcode: 2010Ap&SS.tmp...48G
We present a redetermination of the solar abundances of all available
elements. The new results have very recently been published by
Asplund et al. (Annu. Rev. Astron. Astrophys. 47:481, 2009). The
basic ingredients of this work, the main results and some of their
implications are summarized hereafter.
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Title: The Chemical Composition of the Sun
Authors: Asplund, Martin; Grevesse, Nicolas; Sauval, A. Jacques;
Scott, Pat
2009ARA&A..47..481A Altcode: 2009arXiv0909.0948A
The solar chemical composition is an important ingredient in our
understanding of the formation, structure, and evolution of both the
Sun and our Solar System. Furthermore, it is an essential reference
standard against which the elemental contents of other astronomical
objects are compared. In this review, we evaluate the current
understanding of the solar photospheric composition. In particular,
we present a redetermination of the abundances of nearly all available
elements, using a realistic new three-dimensional (3D), time-dependent
hydrodynamical model of the solar atmosphere. We have carefully
considered the atomic input data and selection of spectral lines, and
accounted for departures from local thermodynamic equilibrium (LTE)
whenever possible. The end result is a comprehensive and homogeneous
compilation of the solar elemental abundances. Particularly noteworthy
findings are significantly lower abundances of C, N, O, and Ne compared
to the widely used values of a decade ago. The new solar chemical
composition is supported by a high degree of internal consistency
between available abundance indicators, and by agreement with
values obtained in the Solar Neighborhood and from the most pristine
meteorites. There is, however, a stark conflict with standard models
of the solar interior according to helioseismology, a discrepancy that
has yet to find a satisfactory resolution.
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Title: Experimental and theoretical radiative decay rates for highly
excited ruthenium atomic levels and the solar abundance of ruthenium
Authors: Fivet, V.; Quinet, P.; Palmeri, P.; Biémont, É.; Asplund,
M.; Grevesse, N.; Sauval, A. J.; Engström, L.; Lundberg, H.; Hartman,
H.; Nilsson, H.
2009MNRAS.396.2124F Altcode: 2009MNRAS.tmp..738F
The solar photospheric abundance of ruthenium is revised on the basis
of a new set of oscillator strengths derived for RuI transitions with
wavelengths in the spectral range 2250-4710 Å. The new abundance value
(in the usual logarithmic scale where the solar hydrogen abundance
is equal to 12.00), A<SUB>Ru</SUB> = 1.72 +/- 0.10, is in agreement
with the most recent meteoritic result, A<SUB>Ru</SUB> = 1.76 +/-
0.03. The accuracy of the transition probabilities, obtained using a
relativistic Hartree-Fock model including core-polarization effects,
has been assessed by comparing the theoretical lifetimes with previous
experimental results. A comparison is also made with new measurements
performed in this work by the time-resolved laser-induced fluorescence
spectroscopy for 10 highly excited odd-parity levels of RuI.
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Title: On the Solar Nickel and Oxygen Abundances
Authors: Scott, Pat; Asplund, Martin; Grevesse, Nicolas; Sauval,
A. Jacques
2009ApJ...691L.119S Altcode: 2008arXiv0811.0815S
Determinations of the solar oxygen content relying on the neutral
forbidden transition at 630 nm depend upon the nickel abundance,
due to a Ni I blend. Here, we rederive the solar nickel abundance,
using the same ab initio three-dimensional hydrodynamic model of the
solar photosphere employed in the recent revision of the abundances
of C, N, O, and other elements. Using 17 weak, unblended lines of
Ni I together with the most accurate atomic and observational data
available, we find log epsilon<SUB>Ni</SUB> = 6.17 ± 0.02(statistical)
± 0.05(systematic), a downward shift of 0.06-0.08 dex relative to
previous abundances based on one-dimensional model atmospheres. We
investigate the implications of the new nickel abundance for studies of
the solar oxygen abundance based on the [O I] 630 nm line in the quiet
Sun. Furthermore, we demonstrate that the oxygen abundance implied
by the recent sunspot spectropolarimetric study of Centeno &
Socas-Navarro needs to be revised downward from log epsilon<SUB>O</SUB>
= 8.86 ± 0.07 to 8.71 ± 0.10. This revision is based on the new
nickel abundance, the application of the best available gf value for
the 630 nm forbidden oxygen line, and a more transparent treatment of
CO formation. Determinations of the solar oxygen content relying on
forbidden lines now appear to converge around log epsilon<SUB>O</SUB>
= 8.7.
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Title: The Solar Chemical Composition
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.
2007SSRv..130..105G Altcode: 2007SSRv..tmp..105G
We present our current knowledge of the solar chemical composition
based on the recent significant downward revision of the solar
photospheric abundances of the most abundant metals. These new solar
abundances result from the use of a 3D hydrodynamic model of the solar
atmosphere instead of the classical 1D hydrostatic models, accounting
for departures from LTE, and improved atomic and molecular data. With
these abundances, the new solar metallicity, Z, decreases to Z=0.012,
almost a factor of two lower than earlier widely used values. We
compare our values with data from other sources and analyse a number
of impacts of these new photospheric abundances. While resolving a
number of longstanding problems, the new 3D-based solar photospheric
composition also poses serious challenges for the standard solar model
as judged by helioseismology.
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Title: The Solar Chemical Composition
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.
2007coma.book..105G Altcode:
We present our current knowledge of the solar chemical composition
based on the recent significant downward revision of the solar
photospheric abundances of the most abundant metals. These new solar
abundances result from the use of a 3D hydrodynamic model of the solar
atmosphere instead of the classical 1D hydrostatic models, accounting
for departures from LTE, and improved atomic and molecular data. With
these abundances, the new solar metallicity, Z, decreases to Z=0.012,
almost a factor of two lower than earlier widely used values. We
compare our values with data from other sources and analyse a number
of impacts of these new photospheric abundances. While resolving a
number of longstanding problems, the new 3D-based solar photospheric
composition also poses serious challenges for the standard solar model
as judged by helioseismology.
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Title: Line formation in solar granulation. VII. CO lines and the
solar C and O isotopic abundances
Authors: Scott, P. C.; Asplund, M.; Grevesse, N.; Sauval, A. J.
2006A&A...456..675S Altcode: 2006astro.ph..5116S
CO spectral line formation in the Sun has long been a source of
consternation for solar physicists, as have the elemental abundances
it seems to imply. We modelled solar CO line formation using a
realistic, ab initio, time-dependent 3D radiative-hydrodynamic model
atmosphere. Results were compared with space-based observations
from the ATMOS space shuttle experiment. We employed weak
<SUP>12</SUP>C<SUP>16</SUP>O, <SUP>13</SUP>C<SUP>16</SUP>O and
<SUP>12</SUP>C<SUP>18</SUP>O lines from the fundamental (Δ v =
1) and first overtone (Δ v = 2) bands to determine the solar
carbon abundance, as well as the <SUP>12</SUP>C/<SUP>13</SUP>C
and <SUP>16</SUP>O/<SUP>18</SUP>O isotopic ratios. A weighted
solar carbon abundance of logɛ_C=8.39 ± 0.05 was found. We
note with satisfaction that the derived abundance is identical to
our recent 3D determination based on C i, [C i], C2 and CH lines,
increasing our confidence in the accuracy of both results. Identical
calculations were carried out using 1D models, but only the 3D
model was able to produce abundance agreement between different
CO lines and the other atomic and molecular diagnostics. Solar
<SUP>12</SUP>C/<SUP>13</SUP>C and <SUP>16</SUP>O/<SUP>18</SUP>O ratios
were measured as 86.8<SUP>+3.9</SUP><SUB>-3.7</SUB> (δ<SUP>13</SUP>C
= 30<SUP>+46</SUP><SUB>-44</SUB>) and 479<SUP>+29</SUP><SUB>-28</SUB>
(δ<SUP>18</SUP>O = 41<SUP>+67</SUP><SUB>-59</SUB>), respectively. These
values may require current theories of solar system formation, such as
the CO self-shielding hypothesis, to be revised. Excellent agreement
was seen between observed and predicted weak CO line shapes, without
invoking micro- or macroturbulence. Agreement breaks down for the
strongest CO lines however, which are formed in very high atmospheric
layers. Whilst the line asymmetries (bisectors) were reasonably
well reproduced, line strengths predicted on the basis of C and O
abundances from other diagnostics were weaker than observed. The
simplest explanation is that temperatures are overestimated in the
highest layers of the 3D simulation. Thus, our analysis supports
the presence of a COmosphere above the traditional photospheric
temperature minimum, with an average temperature of less than 4000
K. This shortcoming of the 3D model atmosphere is not surprising,
given that it was never intended to properly describe such high layers.
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Title: The new solar abundances - Part I: the observations
Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.
2006CoAst.147...76A Altcode:
The new solar abundances have been derived from analyses of the
photospheric spectrum. They result from the use of a 3D hydrodynamical
model of the solar atmosphere instead of the classical 1D hydrostatic
models, accounting for departures from LTE when possible and improved
atomic and molecular data. The new solar abundances are lower than
previously recommended values and the present solar metallicity, Z,
and Z/X, decrease to Z = 0.0122 and Z/X = 0.0165 respectively, almost
a factor of two lower than earlier widely used values. We briefly
discuss the new results for the most abundant elements, show why they
are trustworthy and discuss some implications (see also Montalban et
al. 2006, Part II).
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Title: The solar model problem resurrected
Authors: Asplund, M.; Grevesse, N.; Guedel, M.; Sauval, A. J.
2005astro.ph.10377A Altcode:
The new solar composition, when applied to compute a model of the Sun,
leads to serious disagreement between the predictions of the model
and the observations obtained by helioseismology. New measurements of
the coronal Ne/O abundance ratio in nearby stars using X-ray spectra
typically find high values of Ne/O=0.4 rather than 0.15 normally adopted
for the Sun. Drake & Testa (2005) suggest that this high Ne/O ratio
is appropriate also for the Sun, which would bring the solar models
back in agreement with the helioseismological observations. Here we
present arguments why the high Ne/O ratio is unlikely to be applicable
to the Sun.
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Title: The Solar Chemical Composition
Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.
2005ASPC..336...25A Altcode:
We review our current knowledge of the solar chemical composition
as determined from photospheric absorption lines. In particular we
describe the recent significant revisions of the solar abundances as a
result of the application of a time-dependent, 3D hydrodynamical model
of the solar atmosphere instead of 1D hydrostatic models. This has
decreased the metal content in the solar convection zone by almost a
factor of two compared with the widely used compilation by Anders &
Grevesse (1989). While resolving a number of long-standings problems,
the new 3D-based element abundances also pose serious challenges,
most notably for helioseismology.
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Title: Line formation in solar granulation. IV. [O I], O I and OH
lines and the photospheric O abundance
Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.; Allende Prieto,
C.; Kiselman, D.
2005A&A...435..339A Altcode:
A&A, 417, 751-768 (2004), DOI:10.1051/0004-6361:20034328
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Title: Line formation in solar granulation. VI. [C I], C I, CH and
C<SUB>2</SUB> lines and the photospheric C abundance
Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.; Allende Prieto,
C.; Blomme, R.
2005A&A...431..693A Altcode: 2004astro.ph.10681A
The solar photospheric carbon abundance has been determined from [C
I], C I, CH vibration-rotation, CH A-X electronic and C<SUB>2</SUB>
Swan electronic lines by means of a time-dependent, 3D, hydrodynamical
model of the solar atmosphere. Departures from LTE have been considered
for the C I lines. These turned out to be of increasing importance for
stronger lines and are crucial to remove a trend in LTE abundances
with the strengths of the lines. Very gratifying agreement is found
among all the atomic and molecular abundance diagnostics in spite of
their widely different line formation sensitivities. The mean value
of the solar carbon abundance based on the four primary abundance
indicators ([C I], C I, CH vibration-rotation, C<SUB>2</SUB> Swan)
is log ɛ<SUB>C</SUB> = 8.39 ± 0.05, including our best estimate of
possible systematic errors. Consistent results also come from the CH
electronic lines, which we have relegated to a supporting role due
to their sensitivity to the line broadening. The new 3D based solar C
abundance is significantly lower than previously estimated in studies
using 1D model atmospheres.
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Title: The New Solar Chemical Composition
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.
2005EAS....17...21G Altcode:
We present our current knowledge of the solar chemical composition based
on the recent significant downward revision of the solar photospheric
abundances of the most abundant metals very recently reviewed in detail
by Asplund et al. (2005a). These new solar abundances result from the
use of a 3D hydrodynamical model of the solar atmosphere instead of
the classical 1D hydrostatic models, accounting for departures from
LTE, and improved atomic and molecular data. With these abundances,
the new solar metallicity, Z, and Z/X, decrease to Z = 0.012 and Z/X =
0.0165 respectively, almost a factor of 2 lower than earlier widely
used values. While resolving a number of longstanding problems, the new
3D-based solar photospheric composition also poses serious challenges
for the standard solar model.
---------------------------------------------------------
Title: Line formation in solar granulation. IV. [O I], O I and OH
lines and the photospheric O abundance
Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.; Allende Prieto,
C.; Kiselman, D.
2004A&A...417..751A Altcode: 2003astro.ph.12290A
The solar photospheric oxygen abundance has been determined from
[O I], O I, OH vibration-rotation and OH pure rotation lines by
means of a realistic time-dependent, 3D, hydrodynamical model of
the solar atmosphere. In the case of the O I lines, 3D non-LTE
calculations have been performed, revealing significant departures
from LTE as a result of photon losses in the lines. We derive a solar
oxygen abundance of log ɛ<SUB>O</SUB> = 8.66 ± 0.05. All oxygen
diagnostics yield highly consistent abundances, in sharp contrast
with the results of classical 1D model atmospheres. This low value
is in good agreement with measurements of the local interstellar
medium and nearby B stars. This low abundance is also supported by
the excellent correspondence between lines of very different line
formation sensitivities, and between the observed and predicted line
shapes and center-to-limb variations. Together with the corresponding
down-ward revisions of the solar carbon, nitrogen and neon abundances,
the resulting significant decrease in solar metal mass fraction to Z =
0.0126 can, however, potentially spoil the impressive agreement between
predicted and observed sound speed in the solar interior determined
from helioseismology.
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Title: ISO-SWS calibration and the accurate modelling of cool-star
atmospheres. III. A0 to G2 stars
Authors: Decin, L.; Vandenbussche, B.; Waelkens, K.; Eriksson, C.;
Gustafsson, B.; Plez, B.; Sauval, A. J.
2003A&A...400..695D Altcode: 2002astro.ph..7636D
Vega, Sirius, beta Leo, alpha Car and alpha Cen A belong to a
sample of twenty stellar sources used for the calibration of
the detectors of the Short-Wavelength Spectrometer on board the
Infrared Space Observatory (ISO-SWS). While general problems with
the calibration and with the theoretical modelling of these stars
are reported in {Decin} et al. (\cite{Decin2000b}), each of these
stars is discussed individually in this paper. As demonstrated in
{Decin} et al. (\cite{Decin2000b}), it is not possible to deduce the
effective temperature, the gravity and the chemical composition from
the ISO-SWS spectra of these stars. But since ISO-SWS is absolutely
calibrated, the angular diameter (theta<SUB>d</SUB> ) of these
stellar sources can be deduced from their ISO-SWS spectra, which
consequently yields the stellar radius (R), the gravity-inferred mass
(M<SUB>g</SUB>) and the luminosity (L) for these stars. For Vega,
we obtained theta<SUB>d</SUB> = 3.35 +/- 0.20 mas, R = 2.79 +/-
0.17 R<SUB>sun</SUB>, M<SUB>g</SUB> = 2.54 +/- 1.21 M<SUB>sun</SUB>
and L = 61 +/- 9 L<SUB>sun</SUB>; for Sirius theta<SUB>d</SUB> =
6.17 +/- 0.38 mas, R = 1.75 +/- 0.11 R<SUB>sun</SUB>, M<SUB>g</SUB>
= 2.22 +/- 1.06 M<SUB>sun</SUB> and L = 29 +/- 6 L<SUB>sun</SUB>;
for beta Leo theta<SUB>d</SUB> = 1.47 +/- 0.09 mas, R = 1.75 +/-
0.11 R<SUB>sun</SUB>, M<SUB>g</SUB> = 1.78 +/- 0.46 M<SUB>sun</SUB>
and L = 15 +/- 2 L<SUB>sun</SUB>; for alpha Car theta<SUB>d</SUB> =
7.22 +/- 0.42 mas, R = 74.39 +/- 5.76 R<SUB>sun</SUB>, M<SUB>g</SUB>
= 12.80<SUP>+24.95</SUP><SUB>-6.35</SUB> M<SUB>sun</SUB> and L = 14573
+/- 2268 L<SUB>sun</SUB> and for alpha Cen A theta<SUB>d</SUB> = 8.80
+/- 0.51 mas, R = 1.27 +/- 0.08 R<SUB>sun</SUB>, M<SUB>g</SUB> = 1.35
+/- 0.22 M<SUB>sun</SUB> and L = 1.7 +/- 0.2 L<SUB>sun</SUB>. These
deduced parameters are confronted with other published values and the
goodness-of-fit between observed ISO-SWS data and the corresponding
synthetic spectrum is discussed. <P />Based on observations with ISO,
an ESA project with instruments funded by ESA Member States (especially
the PI countries France, Germany, The Netherlands and the UK) and with
the participation of ISAS and NASA.}\fnmsep\thanks{Appendices A and
B are only available in electronic form at http://www.edpsciences.org}
---------------------------------------------------------
Title: ISO-SWS calibration and the accurate modelling of cool-star
atmospheres. IV. G9 to M2 stars
Authors: Decin, L.; Vandenbussche, B.; Waelkens, C.; Decin, G.;
Eriksson, K.; Gustafsson, B.; Plez, B.; Sauval, A. J.
2003A&A...400..709D Altcode: 2002astro.ph..7653D
A detailed spectroscopic study of 11 giants with spectral type
from G9 to M2 is presented. The 2.38-4.08 mu m wavelength-range of
band 1 of ISO-SWS (Short-Wavelength Spectrometers on board of the
Infrared Space Observatory) in which many different molecules -
with their own dependence on each of the stellar parameters - are
absorbing, enables us to estimate the effective temperature, the
gravity, the microturbulence, the metallicity, the CNO-abundances,
the <SUP>12</SUP>C/<SUP>13</SUP>C-ratio and the angular diameter from
the ISO-SWS data. Using the Hipparcos' parallax, the radius, luminosity
and gravity-inferred mass are derived. The stellar parameters obtained
are in good agreement with other published values, though also some
discrepancies with values deduced by other authors are noted. For a
few stars (delta Dra, xi Dra, alpha Tuc, H Sco and alpha Cet) some
parameters - e.g. the CNO-abundances - are derived for the first
time. By examining the correspondence between different ISO-SWS
observations of the same object and between the ISO-SWS data and
the corresponding synthetic spectrum, it is shown that the relative
accuracy of ISO-SWS in band 1 (2.38-4.08 mu m) is better than 2%
for these high-flux sources. The high level of correspondence between
observations and theoretical predictions, together with a confrontation
of the estimated T<SUB>eff</SUB> (ISO) value with T<SUB>eff</SUB> values
derived from colours - which demonstrates the consistency between V-K,
BC<SUB>K</SUB>, T<SUB>eff</SUB> and theta<SUB>d</SUB> derived from
optical or IR data - proves that both the used MARCS models to derive
the stellar quantities and the flux calibration of the ISO-SWS detectors
have reached a high level of reliability. <P />Based on observations
with ISO, an ESA project with instruments funded by ESA Member States
(especially the PI countries France, Germany, The Netherlands and the
UK) and with the participation of ISAS and NASA. <P />Appendices A-D
are only available in electronic form at http://www.edpsciences.org
---------------------------------------------------------
Title: ISO-SWS calibration and the accurate modelling of cool-star
atmospheres. II. General results
Authors: Decin, L.; Vandenbussche, B.; Waelkens, C.; Eriksson, K.;
Gustafsson, B.; Plez, B.; Sauval, A. J.; Hinkle, K.
2003A&A...400..679D Altcode: 2002astro.ph..7621D
The fine calibration of the ISO-SWS detectors (Infrared Space
Observatory - Short Wavelength Spectrometer) has proven to be a delicate
problem. We therefore present a detailed spectroscopic study in the
2.38-12 mu m wavelength range of a sample of 16 A0-M2 stars used for
the calibration of ISO-SWS. By investigating the discrepancies between
the ISO-SWS data of these sources, the theoretical predictions of their
spectra, the high-resolution FTS-KP (Kitt Peak) spectrum of alpha Boo
and the solar FTS-ATMOS (Atmospheric Trace Molecule Spectroscopy)
spectrum, both calibration problems and problems in computing the
theoretical models and the synthetic spectra are revealed. The
underlying reasons for these problems are sought for and the impact
on the further calibration of ISO-SWS and on the theoretical modelling
is discussed extensively. <P />Based on observations with ISO, an ESA
project with instruments funded by ESA Member States (especially the
PI countries France, Germany, The Netherlands and the UK) and with
the participation of ISAS and NASA. <P />Appendix is only available
in electronic form at http://www.edpsciences.org
---------------------------------------------------------
Title: The Composition of the solar photosphere
Authors: Grevesse, N.; Sauval, A. J.
2002AdSpR..30....3G Altcode:
The Sun is unique because chemical composition data can be derived from
very different layers, from the center to the outermost coronal layers,
using very different techniques like helioseismology, spectroscopy,
particle collection techniques, … Differences in chemical composition
are observed allowing to discover how the different solar layers
evolve. The composition of the solar photosphere, which represents
the composition of the outer convective zone, is the basic reference
source of elemental abundances. We review the current status of our
knowledge of the chemical composition of this layer and compare it
with data from other solar sources as well as with meteoritic data.
---------------------------------------------------------
Title: ISO-SWS calibration and the accurate modelling of cool-star
atmospheres. I. Method
Authors: Decin, L.; Waelkens, C.; Eriksson, K.; Gustafsson, B.; Plez,
B.; Sauval, A. J.; Van Assche, W.; Vandenbussche, B.
2000A&A...364..137D Altcode: 2000astro.ph..8316D
A detailed spectroscopic study of the ISO-SWS data of the red
giant alpha Tau is presented, which enables not only the accurate
determination of the stellar parameters of alpha Tau, but also serves
as a critical review of the ISO-SWS calibration. This study is situated
in a broader context of an iterative process in which both accurate
observations of stellar templates and cool star atmosphere models
are involved to improve the ISO-SWS calibration process as well as the
theoretical modelling of stellar atmospheres. Therefore a sample of cool
stars, covering the whole A0 - M8 spectral classification, has been
observed in order to disentangle calibration problems and problems
in generating the theoretical models and corresponding synthetic
spectrum. By using stellar parameters found in the literature large
discrepancies were seen between the ISO-SWS data and the generated
synthetic spectrum of alpha Tau. A study of the influence of various
stellar parameters on the theoretical models and synthetic spectra,
in conjunction with the Kolmogorov-Smirnov test to evaluate objectively
the goodness-of-fit, enables us to pin down the stellar parameters with
a high accuracy: T<SUB>eff</SUB> = 3850 +/- 70 K, log g = 1.50 +/- 0.15,
M = 2.3 +/- 0.8 M<SUB>sun</SUB>, z = -0.15 +/- 0.20 dex, xi<SUB>t</SUB>
= 1.7 +/- 0.3 km s<SUP>-1</SUP>, <SUP>12</SUP>C/<SUP>13</SUP>C = 10
+/- 1, varepsilon (C) = 8.35 +/- 0.20 dex, varepsilon (N) = 8.35 +/-
0.25 dex, varepsilon (O) = 8.83 +/- 0.15 dex and theta<SUB>d</SUB> =
20.77 +/- 0.83 mas. These atmospheric parameters were then compared
with the results provided by other authors using other methods
and/or spectra. Based on observations with ISO, an ESA project with
instruments funded by ESA Member States (especially the PI countries
France, Germany, the Netherlands and the United Kingdom) and with the
participation of ISAS and NASA.
---------------------------------------------------------
Title: ISO Impact on Stellar Models and Viceversa
Authors: Decin, L.; Waelkens, C.; Eriksson, K.; Gustafsson, B.; Plez,
B.; Sauval, A. J.; van Assche, W.; Vandenbussche, B.
2000ESASP.456..289D Altcode: 2000astro.ph..8362D; 2000ibp..conf..289D
We present a detailed spectroscopic study of a sample of bright,
mostly cool, stars observed with the Short-Wavelength Spectrometer
(SWS) on board ISO, which enables the accurate determination of the
stellar parameters of the cool giants, but also serves as a critical
review of the ISO-SWS calibration.
---------------------------------------------------------
Title: Solar Abundances
Authors: Grevesse, N.; Sauval, A.
2000eaa..bookE1979G Altcode:
What is the Sun made of? This fundamental question only received an
answer about 70 years ago. H N RUSSELL, whose name is associated with
much pioneering research in astrophysics during the first half of this
century as well as with a series of basic work in atomic spectroscopy,
made the first quantitative analysis of the chemical composition of
the SOLAR PHOTOSPHERE in 1929. Using eye estimates ...
---------------------------------------------------------
Title: Abundances of the Elements in the Sun
Authors: Grevesse, N.; Sauval, A. J.
2000orel.conf..261G Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The solar abundance of iron and the photospheric model
Authors: Grevesse, N.; Sauval, A. J.
1999A&A...347..348G Altcode:
Numerous papers on the solar photospheric abundance of iron have
recently been published leading to a longstanding debate concerning
rather different results obtained from the analyses of Fe i lines
and, to a lesser extent, of Fe ii lines. Based on a set of 65 solar
Fe i lines, with accurate transition probabilities as well as new
accurate damping constants, we construct a new empirical photospheric
model. We succeed to reconcile abundance results obtained from low
and high excitation Fe i lines as well as from Fe ii lines and derive
a solar photospheric abundance of iron, A_Fe = 7.50 +/- 0.05, which
perfectly agrees with the meteoritic value. A detailed version of
Table~2 is available in electronic form at the CDS via anonymous ftp
to cdsarc.u-strasbg.fr (130.79.128.5) or at the ORB via anonymous ftp
to ftpserver.oma.be/pub/astro/jacques.
---------------------------------------------------------
Title: VizieR Online Data Catalog: Solar abundance of iron (Grevesse+,
1999)
Authors: Grevesse, N.; Sauval, A. J.
1999yCat..33470348G Altcode:
Numerous papers on the solar photospheric abundance of iron have
recently been published leading to a longstanding debate concerning
rather different results obtained from the analyses of Fe I lines
and, to a lesser extent, of Fe II lines. Based on a set of 65 solar
Fe I lines, with accurate transition probabilities as well as new
accurate damping constants, we construct a new empirical photospheric
model. We succeed to reconcile abundance results obtained from low
and high excitation Fe I lines as well as from Fe II lines and derive
a solar photospheric abundance of iron, A<SUB>Fe</SUB>=7.50+/-0.05,
which perfectly agrees with the meteoritic value. (1 data file).
---------------------------------------------------------
Title: Standard Solar Composition
Authors: Grevesse, N.; Sauval, A. J.
1998SSRv...85..161G Altcode:
We review the current status of our knowledge of the chemical
composition of the Sun, essentially derived from the analysis of the
solar photospheric spectrum. The comparison of solar and meteoritic
abundances confirms that there is a very good agreement between the
two sets of abundances. They are used to construct a Standard Abundance
Distribution.
---------------------------------------------------------
Title: Standard Solar Composition
Authors: Grevesse, N.; Sauval, A. J.
1998sce..conf..161G Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Standard Abundances
Authors: Grevesse, N.; Noels, A.; Sauval, A. J.
1996ASPC...99..117G Altcode: 1996coab.proc..117G
No abstract at ADS
---------------------------------------------------------
Title: A new analysis of the OH radical spectrum from solar infrared
observations.
Authors: Melen, F.; Sauval, A. J.; Grevesse, N.; Farmer, C. B.;
Servais, Ch.; Delbouille, L.; Roland, G.
1995JMoSp.174..490M Altcode:
The solar spectrum offered the opportunity to discover OH lines with
high rotational quantum numbers, which do not appear on laboratory
spectra. On solar absorption spectra, the authors have identified
about 580 lines, among which about 400 were observed for the first
time. They belong to pure rotational transitions in the ground state
(υ = 0→3; J<SUB>max</SUB>″= 48.5), as well as to the (1-0), (2-1),
and (3-2) vibration-rotation bands (J<SUB>max</SUB>″= 32.5). Previous
pure rotation, vibration-rotation, and Λ-doubling data sets related
to the υ = 0 up to 3 levels were fitted simultaneously together with
this new set of data, in order to obtain a very complete and accurate
set of molecular constants for the X<SUP>2</SUP>Π ground state.
---------------------------------------------------------
Title: High excitation Rydberg levels of Fe I from the ATMOS solar
spectrum at 2.5 and 7 μm.
Authors: Schoenfeld, W. G.; Chang, E. S.; Geller, M.; Johansson, S.;
Nave, G.; Sauval, A. J.; Grevesse, N.
1995A&A...301..593S Altcode:
The quadrupole-polarization theory has been applied to the
3d^6^4s(^6^D)4f and 5g subconfigurations of Fe I by a parametric fit,
and the fitted parameters are used to predict levels in the 6g and
6h subconfigurations. Using the predicted values, we have computed
the 4f-6g and 5g-6h transition arrays and made identifications in the
ATMOS infrared solar spectrum. The newly identified 6g and 6h levels,
based on ATMOS wavenumbers, are combined with the 5g levels and found to
agree with the theoretical values with a root mean-squared-deviation of
0.042cm^-1^. Our approach yields a polarizability of 28.07 a_o_^3^and
a quadrupole moment of 0.4360+/-0.0010ea_o_^2^for Fe II, as well as
an improved ionization potential of 63737.700+/-0.010cm^-1^ for Fe I.
---------------------------------------------------------
Title: Charles FIEVEZ; 13 Years of Spectroscopy at the Observatoire
Royal de Bruxelles (1877-1890)
Authors: Sauval, A. J.
1995ASPC...81....3S Altcode: 1995lahr.conf....3S
No abstract at ADS
---------------------------------------------------------
Title: A New Analysis of the OH Radical Spectrum from Solar Infrared
Observations
Authors: Melen, F.; Grevesse, N.; Delbouille, L.; Roland, G.; Servais,
C.; Sauval, A. J.; Farmer, C. B.
1995ASPC...81..320M Altcode: 1995lahr.conf..320M
No abstract at ADS
---------------------------------------------------------
Title: Workshop on Laboratory and Astronomical High Resolution
Spectra : held in Brussels, Belgium 29 August-2 September 1994 in
honour of the 150th birthday of Charles Vievez (1844-1890), the
pioneer of astronomical spectroscopy in Belgium
Authors: Sauval, A. J.; Blomme, R.; Grevesse, N.
1995ASPC...81.....S Altcode: 1995lahr.conf.....S
No abstract at ADS
---------------------------------------------------------
Title: Atomic and Molecular Data in Solar Photospheric Spectroscopy
Authors: Grevesse, N.; Noels, A.; Sauval, A. J.
1995ASPC...81...74G Altcode: 1995lahr.conf...74G
No abstract at ADS
---------------------------------------------------------
Title: Statement
Authors: Sauval, A. J.; Blomme, R.; Grevasse, N.
1995ASPC...81..627S Altcode: 1995lahr.conf..627S
No abstract at ADS
---------------------------------------------------------
Title: Analysis of the 3d 64 s( 6D)4f--5g Supermultiplet of Fe i in
Laboratory and Solar Infrared Spectra
Authors: Johansson, S.; Nave, G.; Geller, M.; Sauval, A. J.; Grevesse,
N.; Schoenfeld, W. G.; Change, E. S.; Farmer, C. B.
1994ApJ...429..419J Altcode: 1994astro.ph..4050J
The combined laboratory and solar analysis of the highly-excited
subconfigurations 4f and 5g of Fe I has allowed us to classify 87
lines of the 4f-5g supermultiplet in the spectral region 2545-2585
cm-1. The level structure of these JK-coupled configurations
is predicted by semiempirical calculations and the quadrupolic
approximation. Semiempirical gf-values have been calculated and
are compared to gf values derived from the solar spectrum. The solar
analysis has shown that these lines, which should be much less sensitive
than lower excitation lines to departures from LTE and to temperature
uncertainties, lead to a solar abundance of iron which is consistent
with the meteoritic value (A_Fe = 7.51).
---------------------------------------------------------
Title: The Sun as a Laboratory Source for IR Molecular Spectroscopy
Authors: Sauval, A. J.; Grevesse, N.
1994IAUS..154..549S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Analysis of Very High Excitation Fe I Lines (4f - 5g) in the
Solar Infrared Spectrum
Authors: Johansson, S.; Nave, G.; Geller, M.; Sauval, A. J.;
Grevesse, N.
1994IAUS..154..543J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Molecules in the Sun and Molecular Data
Authors: Grevesse, Nicolas; Sauval, A. Jacques
1994LNP...428..196G Altcode: 1994mse..conf..196G; 1994IAUCo.146..196G
No abstract at ADS
---------------------------------------------------------
Title: Solar Abundances of C; N; O
Authors: Grevesse, N.; Sauval, A. J.; Blomme, R.
1994IAUS..154..539G Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Line Shifts Asymmetries in the IR Solar Spectrum
Authors: Blomme, R.; Sauval, A. J.; Grevesse, N.
1994IAUS..154..533B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Data for the CN red System from solar lines
Authors: Sauval, A. J.; Blomme, R.; Grevesse, N.
1994msep.conf..107S Altcode: 1994IAUCo.146P.107S
No abstract at ADS
---------------------------------------------------------
Title: A revision of the solar abundance of dysprosium
Authors: Grevesse, N.; Noels, A.; Sauval, A. J.
1993A&A...271..587G Altcode:
The solar abundance of dysprosium is reevaluated from a new analysis of
solar Dy II lines for which new accurate gf-values have recently been
measured by Kusz (1992). The new result, A<SUB>Dy</SUB> = 1.14±0.08,
is in pretty good agreement with the meteoritic value.
---------------------------------------------------------
Title: On the accuracy of CO line positions for high resolution IR
stellar spectroscopy
Authors: Sauval, A. J.; Farrenq, R.; Guelachvili, G.; Grevesse, N.;
Farmer, C. B.; Norton, R. H.
1992A&A...265..355S Altcode:
The paper demonstrates the high accuracy of line positions derived from
improved sets of Dunham coefficients for the four more abundant isotopic
species of carbon monoxide - (C-12)(O-16), (C-13)(O-16), (C-12)(O-18),
and (C-12)(O-17) - which are present in the sun and in cool stellar
atmospheres. These new spectroscopic constants make it possible to
predict very accurate positions of CO lines at any J-values, especially
at very high rotational excitation (up to J around 135). Earlier
proposed identifications of CO lines at large J-values are checked,
and some incorrect identifications in sunspot spectra are found. The
present accurate line positions are also compared with predictions from
other available sets of molecular constants. It is concluded that the
present improved sets of molecular constants are the most appropriate
to all problems of high-resolution stellar and solar spectroscopy at
any J- and v-values, particularly for synthetic spectra of cool stars.
---------------------------------------------------------
Title: Photospheric abundances.
Authors: Grevesse, Nicolas; Noels, A.; Sauval, A. J.
1992ESASP.348..305G Altcode: 1992cscl.work..305G
The authors review the photospheric abundances of the chemical elements
which are observed in the coronal spectrum, in the solar wind and in
solar energetic particle events.
---------------------------------------------------------
Title: Molecular Data from Solar Spectroscopy
Authors: Grevesse, N.; Sauval, A. J.
1992RMxAA..23...71G Altcode:
We show through a few examples how the analysis of molecular transitions
present in the solar visible and infrared spectrum can be used to refine
our knowledge of the molecular constants and to test the accuracy of
available molecular data like transition probabilities and dissociation
energies for a few diatomic molecules. Key words: ATOMIC PROCESSES -
MOLECULAR PROCESSES - SUN: ATMOSPHERE - SUN: SPECTRA
---------------------------------------------------------
Title: Improved Dunham coefficients for CO from infrared solar lines
of high rotational excitation
Authors: Farrenq, R.; Guelachvili, G.; Sauval, A. J.; Grevesse, N.;
Farmer, C. B.
1991JMoSp.149..375F Altcode:
About 4500 unblended CO lines have been selected and their wavenumbers
accurately measured on high resolution solar spectra obtained from
space with the ATMOS Fourier transform spectrometer. Half of these lines
are of high rotational excitation energy and have never been observed
before in the laboratory. Line positions of the fundamental bands of
<SUP>12</SUP>C<SUP>16</SUP>O have been measured up to J = 133, those
of <SUP>13</SUP>C<SUP>16</SUP>O and of <SUP>12</SUP>C<SUP>18</SUP>O
up to J = 103 and 91, respectively. The first overtone bands of
<SUP>12</SUP>C<SUP>16</SUP>O have been measured up to J = 110. These
new solar CO wavenumbers, with an additional selected set of about 14
000 accurate laboratory measurements, have been simultaneously fitted to
the Dunham expression utilizing 10 recently published relations between
isotopically invariant parameters U<SUB>ij</SUB>. The present set of
coefficients reproduces all accurate laboratory positions and our solar
measurements of high rotational excitation with a standard deviation
of about 10<SUP>-5</SUP> cm<SUP>-1</SUP> (300kHz). This new set is
particularly recommended for all high resolution studies of infrared
laboratory and stellar spectra showing CO lines of high J-values. <P
/>It is with deep sorrow that we report the demise of R. H. Norton on
March 22, 1991. His participation in this research was much appreciated.
---------------------------------------------------------
Title: First identification of pure rotation lines of NH in the
infrared solar spectrum
Authors: Geller, M.; Farmer, C. B.; Norton, R. H.; Sauval, A. J.;
Grevesse, N.
1991A&A...249..550G Altcode:
Pure rotation lines of NH of the v = 0 level and v = 1 level are
detected in high-resolution solar spectra obtained from the Atmospheric
Trace Molecule Spectroscopy (ATMOS) experimental observations. It
is pointed out that the identification of the lines is favored by the
typical appearance of the triplet lines of nearly equal intensities. The
observed equivalent widths of these triplet lines are compared with
predicted intensities, and it is observed that these widths are
systematically larger than the predicted values. It is noted that
because these very faint lines are observed in a region where the signal
is very low, a systematic error in the measurements of the equivalent
widths cannot be ruled out; therefore, the disagreement between the
observed and predicted intensities is not considered to be real.
---------------------------------------------------------
Title: Vibration-rotation bands of CH in the solar infrared spectrum
and the solar carbon abundance
Authors: Grevesse, N.; Lambert, D. L.; Sauval, A. J.; van Dishoeck,
E. F.; Farmer, C. B.; Norton, R. H.
1991A&A...242..488G Altcode:
High resolution solar spectra obtained from the ATMOS Fourier Transform
Spectrometer (Spacelab 3 flight on April 29-May 6, 1985) have made
it possible to identify and measure a large number of lines of the
vibration-rotation fundamental bands of the X2 Pi state of CH. From
about 100 lines of the 1-0, 2-1, and 3-2 bands and adopting theoretical
transition probabilities, a solar carbon abundance of 8.60 + or -
0.05 is derived. This value is compared with new results inferred
from other carbon abundance indicators. The final recommended solar
abundance of carbon is 8.60 + or - 0.05.
---------------------------------------------------------
Title: The infrared solar spectrum
Authors: Grevesse, N.; Sauval, A. J.
1991STIN...9413502G Altcode:
The spectrum of the quiet Sun at wavelengths larger than about 1
micrometer (or wavenumbers shorter than 10,000/cm) are described. The
main characteristics of studying the solar spectrum in the infrared
region are summarized. The new high resolution low noise solar spectra
obtained by the Atmospheric Trace Molecule Spectroscopy (ATMOS) Fourier
transform spectrometer experiment on board the Space Shuttle are
considered. Atomic and molecular spectroscopy/line identification are
discussed. Solar observations in the infrared are summarized. Recent
analyses have led to a better understanding of the heterogeneous
structure of the solar outer layers: thermal bifurcation between the
cool photosphere and the hot flux tube chromosphere, convective motions
in the photosphere, oscillations in the photosphere and chromosphere,
magnetic fields and shapes of the flux tubes, etc.
---------------------------------------------------------
Title: The Infrared Solar Spectrum
Authors: Grevesse, N.; Sauval, A. J.
1991isrs.conf..215G Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Identification of solar vibration-rotation lines of NH and
the solar nitrogen abundance
Authors: Grevesse, N.; Lambert, D. L.; Sauval, A. J.; van Dishoeck,
E. F.; Farmer, C. B.; Norton, R. H.
1990A&A...232..225G Altcode:
High resolution solar spectra obtained from the ATMOS Fourier Transform
Spectrometer (Spacelab 3 flight on April 29 - May 6, 1985) made it
possible to detect for the first time vibration-rotation lines of NH
from the X3 Sigma(-) state near 3 microns. Using recent theoretical
results for the transition probabilities of 23 selected measured lines
of the 1-0 and 2-1 bands, a solar abundance of nitrogen of 8.06 + or -
0.07 is derived. This value is compared with the result derived from
N I lines and agrees with the abundance obtained from the 3s-3p, 3p-3d
and 3s-prime - 3p-prime transitions, A(N) = 8.00 + or - 0.09. The final
recommended solar abundance of nitrogen is A(N) = 8.00 + or - 0.05.
---------------------------------------------------------
Title: A new analysis of the vibration-rotation spectrum of CH from
solar spectra
Authors: Melen, F.; Grevesse, N.; Sauval, A. J.; Farmer, C. B.;
Norton, R. H.; Bredohl, H.; Dubois, I.
1989JMoSp.134..305M Altcode:
In the solar spectrum, CH vibration-rotation lines are excited to
higher vibrational and much higher rotational quantum numbers than in
any laboratory source. We have observed, for the first time, a very
large number of new lines (1-0 and 2-1 up to J = 34.5, 3-2 up to J =
31.5, and even 4-3, never seen before, up to J = 24.5) on solar spectra
obtained from space, with the ATMOS-SL3 instrument. A total of 558
lines have been used to derive new accurate molecular constants for
the X<SUP>2</SUP>Π ground state of CH.
---------------------------------------------------------
Title: Concentrations of hydrogen chloride and hydrogen fluoride
measured during the MAP/GLOBUS campaign of September 1983
Authors: Zander, R.; Roland, G.; Delbouille, L.; Sauval, A. J.;
Marché, P.; Karcher, F.; Amoudei, M.; Dufour, B.
1987P&SS...35..665Z Altcode:
Within the context of the MAP/GLOBUS campaign of September 1983,
several trace species have been observed by absorption spectroscopy
at the two ground stations of the Jungfraujoch, Switzerland (3580
m altitude) and the Observatoire de Haute-Provence, France (1905 m
altitude). The results obtained for HCl and for HF, expressed in terms
of mean integrated columns above these sites are: Jungfraujoch: (2.1 ±
0.2) E15 mol cm <SUP>-2</SUP> HCl (4.8 ± 0.2) E14 mol cm <SUP>-2</SUP>
HF Haute-Provence: (2.6 ± 0.2) E15 mol cm <SUP>-2</SUP> HCl. Taking
into account the difference in the altitude of the two stations,
the reported HC1 results are in agreement to within their respective
uncertainties. The integrated column density of HCl and HF above 11 km
altitude, deduced from airplane observations on 9 September 1983, are:
(1.65 ± 0.25) E15 mol cm <SUP>-2</SUP> HCl above 11 km (3.7 ± 1.7)
E14 mol cm <SUP>-2</SUP> HF above 10 km supporting satisfactorily the
ground measurements.
---------------------------------------------------------
Title: Diatomic molecules in the solar infrared spectrum from
ATMOS-SL3 highresolution observations.
Authors: Grevesse, Nicolas; Sauval, A. J.; Farmer, C. B.; Norton, R. H.
1987LIACo..27..111G Altcode: 1987oahp.proc..111G
The ATMOS Fourier Transform Spectrometer has observed, for the first
time, the solar infrared spectrum, from 2 to 16 microns, free of
any telluric absorption. A very large number of molecular lines are
present on these high quality spectra: vibration-rotation lines of CO
(Delta-v = 1 and 2; including the isotopic species C-13, O-18 and O-17),
CH, NH, OH and pure rotation lines of OH. The analysis of these lines
will allow to derive accurate values for the solar abundances of C,
N and O and the isotopic ratios C-13/C-12, O-18/O-16, and O-17/O-16,
to test the photospheric model from high to deep layers, to test the
electric dipole moment functions of the different molecules and to
derive much better molecular constants for CH.
---------------------------------------------------------
Title: Identification of vibration-rotation lines of CH in the solar
infrared spectrum
Authors: Sauval, A. J.; Grevesse, N.
1985AExpr...1..153S Altcode:
Transitions of the fundamental band of CH have recently been measured
with very high accuracy by Lubic and Amano (1984). The lines are
shown to be present in the solar infrared spectrum (2580 - 2940
cm<SUP>-1</SUP>). The role these lines could play in solar and stellar
spectroscopy is discussed.
---------------------------------------------------------
Title: The Interest of Simultaneous Spectral and Spatial High
Resolution Spectroscopy in the Infrared
Authors: Delbouille, L.; Grevesse, N.; Sauval, A. J.
1985LNP...233..108D Altcode: 1985hrsp.proc..108D
Up to the present, small scale structures on the sun have mostly been
studied through observations made in the visible and ultraviolet. After
having recalled some of the main advantages of infrared observations,
the authors give a few samples of high spectral resolution/low noise
solar spectra now routinely obtained in this spectral range by using
Fourier transform spectrometers. The authors then show that such high
spectral resolution spectra could be obtained in short period of time
and for small scale solar structures, using a LEST type collector.
---------------------------------------------------------
Title: The interest of simultaneous spectral and spatial high
resolution spectroscopy in the infrared.
Authors: Delbouille, L.; Grevesse, N.; Sauval, A. J.
1985CoORB..80.....D Altcode:
After having recalled some of the main advantages of infrared
observations, the authors give a few samples of high spectral
resolution/low noise solar spectra now routinely obtained in this
spectral range by using Fourier transform spectrometers. They then show
that such high resolution spectra could be obtained in a short period of
time and for small-scale solar structures, using a LEST type collector.
---------------------------------------------------------
Title: An analysis of vibration-rotation lines of OH in the solar
infrared spectrum
Authors: Grevesse, N.; Sauval, A. J.; van Dishoeck, E. F.
1984A&A...141...10G Altcode:
High resolution solar spectra have permitted the measurement with great
accuracy of equivalent widths of vibration-rotation lines of OH in the
X2Pi state near 3-micron wavelength. Using recent theoretical results
for the transition probabilities, a solar oxygen abundance of (8.93 +
or - 0.02) is derived which is in perfect agreement with the abundance
deduced from the OH pure rotation lines. The solar abundance of oxygen
is therefore A(O) = 8.92 + or - 0.035, as inferred from the analysis
of 43 vibration-rotation lines and 81 pure rotation lines of the OH
molecule. It is confirmed that the dipole moment function of Werner,
Rosmus and Reinsch (1983) together with the Holweger-Mueller (1974)
solar atmosphere model are to be preferred in the analysis of the data.
---------------------------------------------------------
Title: A set of partition functions and equilibrium constants for
300 diatomic molecules of astrophysical interest
Authors: Sauval, A. J.; Tatum, J. B.
1984ApJS...56..193S Altcode:
Polynomial developments for partition functions and equilibrium
constants of 300 diatomic molecules and of relevant atoms are given for
a temperature range from 1000 to 9000K. All molecular spectroscopic
data, with a few exceptions, are derived from the book by Huber and
Herzberg in order to lead to a homogeneous set of data.
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Title: The pure rotation spectrum of OH and the solar oxygen abundance
Authors: Sauval, A. J.; Grevesse, N.; Zander, R.; Brault, J. W.;
Stokes, G. M.
1984ApJ...282..330S Altcode:
High-resolution low-noise spectroscopic observations of the sun obtained
in the 10.6-13-micron range using the Fourier-transform spectrometer at
Kitt Peak National Observatory are reported. About 100 pure rotation
lines of the X 2Pi electronic state of OH with v = 0, 1, 2, and 3
are identified and characterized. The data are presented in tables
and graphs and used to calculate the solar O abundance as 8.91 + or -
0.01 (in agreement with Lambert, 1978). Agreement is also found with
the electric-dipole-moment function of Werner et al. (1983) and the
photospheric model of Holweger and Mueller (1974).
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Title: Molecules in red-giant stars. I - Column densities in models
for K and M stars
Authors: Johnson, H. R.; Sauval, A. J.
1982A&AS...49...77J Altcode:
Weighted column densities have been calculated for neutral atoms
and ions of most elements and for many molecules in 6 selected model
atmospheres of red-giant stars (2500 ≤ T<SUB>eff</SUB> ≤ 4000 K)
with solar composition. These comprise the most abundant molecules from
a total of about 1600 compounds analyzed. This calculation provides
a guide for identification of new molecular bands in cool stellar
spectra and for laboratory analysis of those molecules of stellar
interest which are as yet not studied spectroscopically.
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Title: Infrared bands of C2 in the solar photospheric spectrum
Authors: Brault, J. W.; Testerman, L.; Grevesse, N.; Sauval, A. J.;
Delbouille, L.; Roland, G.
1982A&A...108..201B Altcode:
Lines of the C<SUB>2</SUB> Phillips system have been successfully
searched for on new tracings of high resolution solar spectra. From a
rather large number of lines of the (0,0), (1,0), and (0, 1) bands,
we derive empirical values for the band oscillator strengths:
f<SUB>00</SUB> = 1.41 10<SUP>-3</SUP>, f<SUB>10</SUB> = 1.38
10<SUP>-3</SUP>, and f<SUB>01</SUB> = 1.12 10<SUP>-3</SUP>. These
solar f-values are discussed in section 3.1 and compared with recent
laboratory data. <P />For the Ballik-Ramsay system, only a few
unblended solar lines have been available, from which we deduced 0.6
10<SUP>-3</SUP> ≪ f<SUB>00</SUB> ≪ 1.2 10<SUP>-3</SUP>.
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Title: Molecular Data Needed in Stellar Spectroscopy Studies
Authors: Grevesse, N.; Sauval, A. J.
1980LIACo..21..289G Altcode: 1980smsl.conf..289G
No abstract at ADS
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Title: Theoretical molecular abundances in cool stellar models
Authors: Johnson, H. R.; Sauval, A. J.
1980LIACo..21..201J Altcode: 1980smsl.conf..201J
No abstract at ADS
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Title: A search for faint molecular lines in the solar photospheric
spectrum
Authors: Sauval, A. J.; Biemont, E.; Grevesse, N.; Zander, R.
1980LIACo..21..235S Altcode: 1980smsl.conf..235S
No abstract at ADS
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Title: Predicted presence and tentative identification of new
molecules in the pure S star R Cyg.
Authors: Sauval, A. J.
1978A&A....62..295S Altcode:
A new approach to the problem of the identification of molecular
features observed in the spectra of pure S stars has been
attempted. From calculations of the chemical equilibrium in cool
stellar models, including a very large number of compounds, a first
selection has been made among molecules which ought to be present in
S stars. On the basis of these predictions, a search has been made
for bands of these new compounds in spectrograms of R Cyg recently
obtained by Wyckoff and Wehinger. The presence of some new molecules,
such as HfO and TaO, in this pure S star is proposed, but the lack of
complete laboratory data and the existence of numerous blends in the
stellar spectrum render very difficult any definite identification.
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Title: Conditions d'observation des Comètes périodiques Encke et
Grigg-Skjellerup en 1977
Authors: Debehogne, H.; Sauval, A. J.
1976C&T....92..333D Altcode:
No abstract at ADS
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Title: Influence of Uncertainties of Molecular Data upon the
Determination of Abundances in Cool Stars
Authors: Sauval, A. J.
1976IAUS...72...21S Altcode:
No abstract at ADS
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Title: The CO fundamental bands in the solar spectrum.
Authors: Muller, C.; Sauval, A. J.
1975A&A....39..445M Altcode:
The result of a study of CO lines in the delta v equals 1 bands in
the solar disk spectrum is presented. Recently, the photospheric
spectrum has been recorded using a balloon-borne spectrometer from
40 km altitude. From a comparison between the observed and synthetic
solar spectra, an agreement is shown using the best available solar
and molecular data. Results are discussed and compared with other
investigations in order to explain an apparent discrepancy between
previous results.
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Title: The CO fundamental bands in the solar spectrum
Authors: Muller, C.; Sauval, A. J.
1975STIN...7530990M Altcode:
The results of a study of CO lines in the * delta v equals 1 bands in
the solar disk spectrum are presented. The photospheric spectrum is
recorded using a balloon-borne spectrometer from 40 km altitude. From
a comparison between the observed and synthetic solar spectra are
compared. An agreement is shown using the best available solar
and molecular data. Results are discussed and compared with other
investigations and explain an apparent discrepancy among previous
results.
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Title: K. R. Lang - Astrophysical Formulae
Authors: Sauval, A. J.
1975C&T....91..320S Altcode:
No abstract at ADS
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Title: A Study of Molecular Lines in the Solar Photospheric Spectrum
Authors: Grevesse, N.; Sauval, A. J.
1973A&A....27...29G Altcode:
Summary. We have analysed the behaviour of lines of C2, CH, CN, MgH,
NH and OH in the solar photospheric spectrum. Recently observed
profiles of these lines have been measured and compared with
profiles computed using recent solar and molecular data. The main
results of this comparison are (I) there is good agreement between
observed and calculated profiles for most of the molecular bands;
(11) but large disagreements appear in the case of CN and MgH; these
discrepancies cannot be explained satisfactorily, although different
possible suggestions are investigated. In the Appendix, a review of
the different experimental band oscillator strengths is presented
and mean laboratory values are proposed. Key words: solar spectrum -
molecular lines - molecular oscillator strengths
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Title: A Search for CH+ in the Solar Photospheric Spectrum
Authors: Grevesse, N.; Sauval, A. J.
1971A&A....14..477G Altcode:
We present the results of a search for lines of CH+ (A1H - X1 +
transition) in the solar photospheric spectrum. We conclude that if CH+
is present, the equivalent widths of the most intense lines cannot
exceed 2 mA. An empirical solar !00-value is derived and compared
with a laboratory value and other available astrophysical values. Some
possible reasons are given for explaining the large discrepancy between
laboratory and astrophysical !00-values - Key words: solar spectrum -
molecules - oscillator strengths
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Title: Oscillator strengths for SiH and SiH<SUP>+</SUP> deduced from
the solar spectrum.
Authors: Grevesse, N.; Sauval, A. J.
1971JQSRT..11...65G Altcode:
No abstract at ADS
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Title: Identification of SiH~ in the Solar Photospheric Spectrum
Authors: Grevesse, N.; Sauval, A. J.
1970A&A.....9..232G Altcode:
We present the first convincing identification of a molecular ion in a
stellar atmosphere: the absorption band spectrum of SiH+ (transition
A 1H - X i +) in the solar photospheric spectrum. Values of the band
oscillator strengths have been deduced for two bands: too = 0.0005
and !oi = 0.0004.
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Title: Identification of SiH Lines in the Solar Disk Spectrum
Authors: Sauval, A. J.
1969SoPh...10..319S Altcode:
A new investigation of the presence of SiH lines in the solar disk
spectrum has been performed. It may be concluded that molecular
absorption lines of SiH are present in the disk spectrum with maximum
equivalent widths of about 2 mÅ. A value of the oscillator strength
of SiH has been derived (f<SUB>00</SUB> = 0.0008 ± 0.0004).
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Title: The solar continuum from 900 to 130 000 Å and the photospheric
temperature model
Authors: Sauval, A.
1968SoPh....3...89S Altcode:
In order to obtain a better agreement between observed and computed
values of the solar intensity, an improved temperature distribution is
deduced for the range 0.02<τ0< 10. The intensity observations
here considered refer to the wavelength region between λ 1980 and λ
129 500, and the center-limb variations generally go down to cosθ =
0.1. The improved model, given in Figure 4 and Table II, differs rather
little from the Utrecht 1964 model, used here as a reference.
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Title: Le projet West Ford
Authors: Sauval, A.
1963C&T....79...12S Altcode:
No abstract at ADS