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Eriksson, Kjell
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Van Eck, S., Neyskens, P., Jorissen, A., Plez, B., Edvardsson, B., Eriksson, K., . . . Nordlund, Å. (2017). A grid of MARCS model atmospheres for late-type stars II. S stars and their properties. Astronomy and Astrophysics, 601, Article ID A10.
Open this publication in new window or tab >>A grid of MARCS model atmospheres for late-type stars II. S stars and their properties
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2017 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 601, article id A10Article in journal (Refereed) Published
Abstract [en]

S-type stars are late-type giants whose atmospheres are enriched in carbon and s-process elements because of either extrinsic pollution by a binary companion or intrinsic nucleosynthesis and dredge-up on the thermally-pulsing asymptotic giant branch. A grid of MARCS model atmospheres has been computed for S stars, covering the range 2700 <= T-eff (K) <= 4000, 0.50 <= C/O less than or similar to 0.99, 0 <= log g <= 5, [Fe/H] = 0., -0.5 dex, and [s/Fe] = 0, 1, and 2 dex (where the latter quantity refers to the global overabundance of s-process elements). The MARCS models make use of a new ZrO line list. Synthetic spectra computed from these models are used to derive photometric indices in the Johnson and Geneva systems, as well as TiO and ZrO band strengths. A method is proposed to select the model best matching any given S star, a non-trivial operation since the grid contains more than 3500 models covering a five-dimensional parameter space. The method is based on the comparison between observed and synthetic photometric indices and spectral band strengths, and has been applied on a vast subsample of the Henize sample of S stars. Our results confirm the old claim by Piccirillo (1980, MNRAS, 190, 441) that ZrO bands in warm S stars (T-eff > 3200 K) are not caused by the C /O ratio being close to unity, as traditionally believed, but rather by some Zr overabundance. The TiO and ZrO band strengths, combined with V - K and J - K photometric indices, are used to select T-eff, C/O, [Fe/H] and [s/Fe]. The Geneva U - B1 and B2 - V1 indices (or any equivalent) are good at selecting the gravity. The defining spectral features of dwarf S stars are outlined, but none is found among the Henize S stars. More generally, it is found that, at T-eff = 3200 K, a change of C/O from 0.5 to 0.99 has a strong impact on V - K (2 mag). Conversely, a range of 2 mag in V - K corresponds to a 200 K shift along the (T-eff, V - K) relationship (for a fixed C/O value). Hence, the use of a (T-eff, V - K) calibration established forMstars will yield large errors for S stars, so that a specific calibration must be used, as provided in the present paper. Using the atmospheric parameters derived by our method for the sample of Henize S stars, we show that the extrinsic-intrinsic dichotomy among S stars reveals itself very clearly as a bimodal distribution in the e ff ective temperatures. Moreover, the increase of s-process element abundances with increasing C/O ratios and decreasing temperatures is apparent among intrinsic stars, confirming theoretical expectations.

Place, publisher, year, edition, pages
EDP Sciences, 2017
Keywords
stars: atmospheres, stars: fundamental parameters, stars: late-type, stars: AGB and post-AGB, stars: abundances, stars: general
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-327051 (URN)10.1051/0004-6361/201525886 (DOI)000402313500010 ()
Available from: 2017-08-03 Created: 2017-08-03 Last updated: 2017-08-03Bibliographically approved
Jonsson, H., Ryde, N., Nordlander, T., Rhodin, A. P., Hartman, H., Jonsson, P. & Eriksson, K. (2017). Abundances of disk and bulge giants from high-resolution optical spectra I. O, Mg, Ca, and Ti in the solar neighborhood and Kepler field samples. Astronomy and Astrophysics, 598, Article ID A100.
Open this publication in new window or tab >>Abundances of disk and bulge giants from high-resolution optical spectra I. O, Mg, Ca, and Ti in the solar neighborhood and Kepler field samples
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2017 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 598, article id A100Article in journal (Refereed) Published
Abstract [en]

Context. The Galactic bulge is an intriguing and significant part of our Galaxy, but it is hard to observe because it is both distant and covered by dust in the disk. Therefore, there are not many high-resolution optical spectra of bulge stars with large wavelength coverage, whose determined abundances can be compared with nearby, similarly analyzed stellar samples. Aims. We aim to determine the diagnostically important alpha elements of a sample of bulge giants using high-resolution optical spectra with large wavelength coverage. The abundances found are compared to similarly derived abundances from similar spectra of similar stars in the local thin and thick disks. In this first paper we focus on the solar neighborhood reference sample. Methods. We used spectral synthesis to derive the stellar parameters as well as the elemental abundances of both the local and bulge samples of giants. We took special care to benchmark our method of determining stellar parameters against independent measurements of effective temperatures from angular diameter measurements and surface gravities from asteroseismology. Results. In this first paper we present the method used to determine the stellar parameters and elemental abundances, evaluate them, and present the results for our local disk sample of 291 giants. Conclusions. When comparing our determined spectroscopic temperatures to those derived from angular diameter measurements, we reproduce these with a systematic difference of + 10 K and a standard deviation of 53 K. The spectroscopic gravities reproduce those determined from asteroseismology with a systematic off set of + 0.10 dex and a standard deviation of 0.12 dex. When it comes to the abundance trends, our sample of local disk giants closely follows trends found in other works analyzing solar neighborhood dwarfs, showing that the much brighter giant stars are as good abundance probes as the often used dwarfs.

Place, publisher, year, edition, pages
EDP SCIENCES S A, 2017
Keywords
solar neighborhood, Galaxy: evolution, stars: abundances
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-320502 (URN)10.1051/0004-6361/201629128 (DOI)000394465000099 ()
Funder
Lars Hierta Memorial FoundationSwedish Research Council, 20114206 2014-5640 2015-4842
Available from: 2017-04-20 Created: 2017-04-20 Last updated: 2017-04-20Bibliographically approved
Wittkowski, M., Hofmann, K.-H. -., Höfner, S., Le Bouquin, J. B., Nowotny, W., Paladini, C., . . . Weigelt, G. (2017). Aperture synthesis imaging of the carbon AGB star R Sculptoris Detection of a complex structure and a dominating spot on the stellar disk. Astronomy and Astrophysics, 601, Article ID A3.
Open this publication in new window or tab >>Aperture synthesis imaging of the carbon AGB star R Sculptoris Detection of a complex structure and a dominating spot on the stellar disk
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2017 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 601, article id A3Article in journal (Refereed) Published
Abstract [en]

Aims. We present near-infrared interferometry of the carbon-rich asymptotic giant branch (AGB) star R Sculptoris (R Scl). Methods. We employ medium spectral resolution K-band interferometry obtained with the instrument AMBER at the Very Large Telescope Interferometer (VLTI) and H-band low spectral resolution interferometric imaging observations obtained with the VLTI instrument PIONIER. We compare our data to a recent grid of dynamic atmosphere and wind models. We compare derived fundamental parameters to stellar evolution models. Results. The visibility data indicate a broadly circular resolved stellar disk with a complex substructure. The observed AMBER squared visibility values show drops at the positions of CO and CN bands, indicating that these lines form in extended layers above the photosphere. The AMBER visibility values are best fit by a model without a wind. The PIONIER data are consistent with the same model. We obtain a Rosseland angular diameter of 8.9 +/- 0.3 mas, corresponding to a Rosseland radius of 355 +/- 55 R-Theta, an effective temperature of 2640 +/- 80 K, and a luminosity of log L/L-Theta = 3.74 +/- 0.18. These parameters match evolutionary tracks of initial mass 1.5 +/- 0.5 M-Theta and current mass 1.3 +/- 0.7 M-Theta. The reconstructed PIONIER images exhibit a complex structure within the stellar disk including a dominant bright spot located at the western part of the stellar disk. The spot has an H- band peak intensity of 40% to 60% above the average intensity of the limb-darkening-corrected stellar disk. The contrast between the minimum and maximum intensity on the stellar disk is about 1:2.5. Conclusions. Our observations are broadly consistent with predictions by dynamic atmosphere and wind models, although models with wind appear to have a circumstellar envelope that is too extended compared to our observations. The detected complex structure within the stellar disk is most likely caused by giant convection cells, resulting in large-scale shock fronts, and their effects on clumpy molecule and dust formation seen against the photosphere at distances of 2-3 stellar radii.

Place, publisher, year, edition, pages
EDP Sciences, 2017
Keywords
techniques: interferometric, stars: AGB and post-AGB, stars: atmospheres, stars: fundamental parameters, stars: mass-loss, stars: individual: R Scl
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-327053 (URN)10.1051/0004-6361/201630214 (DOI)000402313500003 ()
Available from: 2017-08-03 Created: 2017-08-03 Last updated: 2017-08-03Bibliographically approved
Liljegren, S., Höfner, S., Eriksson, K. & Nowotny, W. (2017). Pulsation-induced atmospheric dynamics in M-type AGB stars: Effects on wind properties, photometric variations and near-IR CO line profiles. Astronomy and Astrophysics, 606, Article ID A6.
Open this publication in new window or tab >>Pulsation-induced atmospheric dynamics in M-type AGB stars: Effects on wind properties, photometric variations and near-IR CO line profiles
2017 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 606, article id A6Article in journal (Refereed) Published
Abstract [en]

Context. Wind-driving in asymptotic giant branch (AGB) stars is commonly attributed to a two-step process. First, matter in the stellar atmosphere is levitated by shock waves, induced by stellar pulsation, and second, this matter is accelerated by radiation pressure on dust, resulting in a wind. In dynamical atmosphere and wind models the effects of the stellar pulsation are often simulated by a simplistic prescription at the inner boundary.

Aims. We test a sample of dynamical models for M-type AGB stars, for which we kept the stellar parameters fixed to values characteristic of a typical Mira variable but varied the inner boundary condition. The aim was to evaluate the effect on the resulting atmosphere structure and wind properties. The results of the models are compared to observed mass-loss rates and wind velocities, photometry, and radial velocity curves, and to results from 1D radial pulsation models. The goal is to find boundary conditions which give realistic atmosphere and wind properties.

Methods. Dynamical atmosphere models are calculated, using the DARWIN code for different combinations of photospheric velocities and luminosity variations. The inner boundary is changed by introducing an offset between maximum expansion of the stellar surface and the luminosity and/or by using an asymmetric shape for the luminosity variation. Ninety-nine different combinations of theses two changes are tested.

Results. The model atmospheres are very sensitive to the inner boundary. Models that resulted in realistic wind velocities and mass-loss rates, when compared to observations, also produced realistic photometric variations. For the models to also reproduce the characteristic radial velocity curve present in Mira stars (derived from CO Delta v = 3 lines), an overall phase shift of 0.2 between the maxima of the luminosity and radial variation had to be introduced. This is a larger phase shift than is found by 1D radial pulsation models.

Conclusions. We find that a group of models with different boundary conditions (29 models, including the model with standard boundary conditions) results in realistic velocities and mass-loss rates, and in photometric variations. To achieve the correct line splitting time variation a phase shift is needed.

Keywords
stars: AGB and post-AGB, stars: atmospheres, stars: winds, outflows, infrared: stars, line: profiles
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-337752 (URN)10.1051/0004-6361/201731137 (DOI)000412873800006 ()
Funder
Swedish Research Council
Available from: 2018-01-12 Created: 2018-01-12 Last updated: 2018-04-10Bibliographically approved
Rau, G., Hron, J., Paladini, C., Aringer, B., Eriksson, K., Marigo, P., . . . Grellmann, R. (2017). The adventure of carbon stars: Observations and modeling of a set of C-rich AGB stars. Astronomy and Astrophysics, 600, Article ID A92.
Open this publication in new window or tab >>The adventure of carbon stars: Observations and modeling of a set of C-rich AGB stars
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2017 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 600, article id A92Article in journal (Refereed) Published
Abstract [en]

Context. Modeling stellar atmospheres is a complex and intriguing task in modern astronomy. A systematic comparison of models with multi-technique observations is the only efficient way to constrain the models. Aims. We intend to perform self-consistent modeling of the atmospheres of six carbon-rich AGB stars (R Lep, R Vol, Y Pav, AQ Sgr, U Hya, and X TrA) with the aim of enlarging the knowledge of the dynamic processes occurring in their atmospheres. Methods. We used VLTI/MIDI interferometric observations, in combination with spectro-photometric data, and compared them with self-consistent, dynamic model atmospheres. Results. We found that the models can reproduce spectral energy distribution (SED) data well at wavelengths longer than 1 mu m, and the interferometric observations between 8 mu m and 10 mu m. Discrepancies observed at wavelengths shorter than 1 mu m in the SED, and longer than 10 mu m in the visibilities, could be due to a combination of data- and model-related effects. The models best fitting the Miras are significantly extended, and have a prominent shell-like structure. On the contrary, the models best fitting the non-Miras are more compact, showing lower average mass loss. The mass loss is of episodic or multi-periodic nature but causes the visual amplitudes to be notably larger than the observed ones. A number of stellar parameters were derived from the model fitting: T-Ross, L-Ross, M, C/O, and. M. Our findings agree well with literature values within the uncertainties. TRoss, and LRoss are also in good agreement with the temperature derived from the angular diameter T(theta((V-K))) and the bolometric luminosity from the SED fitting L-bol, except for AQ Sgr. The possible reasons are discussed in the text. Finally, theta(Ross) and theta((V-K)) agree with one another better for the Miras than for the non-Miras targets, which is probably connected to the episodic nature of the latter models. We also located the stars in the H-R diagram, comparing them with evolutionary tracks. We found that the main derived properties (L, T-eff, C/O ratios and stellar masses) from the model fitting are in good agreement with TP-AGB evolutionary calculations for carbon stars carried out with the COLIBRI code.

Place, publisher, year, edition, pages
EDP SCIENCES S A, 2017
Keywords
stars: AGB and post-AGB, stars: atmospheres, stars: mass-loss, stars: carbon, techniques: interferometric, techniques: high angular resolution
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-324342 (URN)10.1051/0004-6361/201629337 (DOI)000400754000048 ()
Funder
EU, European Research Council, 615604
Available from: 2017-06-14 Created: 2017-06-14 Last updated: 2017-06-14Bibliographically approved
Liljegren, S., Höfner, S., Nowotny, W. & Eriksson, K. (2016). Dust-driven winds of AGB stars: The critical interplay of atmospheric shocks and luminosity variations. Astronomy and Astrophysics, 589, Article ID A130.
Open this publication in new window or tab >>Dust-driven winds of AGB stars: The critical interplay of atmospheric shocks and luminosity variations
2016 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 589, article id A130Article in journal (Refereed) Published
Abstract [en]

Context. Winds of AGB stars are thought to be driven by a combination of pulsation-induced shock waves and radiation pressure on dust. In dynamic atmosphere and wind models, the stellar pulsation is often simulated by prescribing a simple sinusoidal variation in velocity and luminosity at the inner boundary of the model atmosphere.

Aims. We experiment with different forms of the luminosity variation in order to assess the effects on the wind velocity and mass-loss rate, when progressing from the simple sinusoidal recipe towards more realistic descriptions. This will also give an indication of how robust the wind properties derived from the dynamic atmosphere models are.

Methods. Using state-of-the-art dynamical models of C-rich AGB stars, a range of different asymmetric shapes of the luminosity variation and a range of phase shifts of the luminosity variation relative to the radial variation are tested. These tests are performed on two stellar atmosphere models. The first model has dust condensation and, as a consequence, a stellar wind is triggered, while the second model lacks both dust and wind.

Results. The first model with dust and stellar wind is very sensitive to moderate changes in the luminosity variation. There is a complex relationship between the luminosity minimum, and dust condensation: changing the phase corresponding to minimum luminosity can either increase or decrease mass-loss rate and wind velocity. The luminosity maximum dominates the radiative pressure on the dust, which in turn, is important for driving the wind. An earlier occurrence of the maximum, with respect to the propagation of the pulsation-induced shock wave, then increases the wind velocity, while a later occurrence leads to a decrease. These effects of changed luminosity variation are coupled with the dust formation. In contrast there is very little change to the structure of the model without dust.

Conclusions. Changing the luminosity variation, both by introducing a phase shift and by modifying the shape, influences wind velocity and the mass-loss rate. To improve wind models it would probably be desirable to extract boundary conditions from 3D dynamical interior models or stellar pulsation models.

Keywords
stars: late-type, stars: AGB and post-AGB, stars: atmospheres, stars: winds, outflows, infrared: stars, line: profiles
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-298682 (URN)10.1051/0004-6361/201527885 (DOI)000375318300142 ()
Funder
Swedish Research Council
Available from: 2016-07-07 Created: 2016-07-06 Last updated: 2018-04-10Bibliographically approved
Eriksson, K., Nowotny, W., Höfner, S. & Aringer, B. (2015). A New Library of Synthetic Spectra and Photometry for Evolved C Stars. In: WHY GALAXIES CARE ABOUT AGB STARS III: A CLOSER LOOK IN SPACE AND TIME. Paper presented at Conference on Why Galaxies Care About AGB Stars III: A Closer Look in Space and Time, JUL 28-AUG 01, 2014, Univ Vienna, Vienna, AUSTRIA (pp. 111-112). ASTRONOMICAL SOC PACIFIC, 497
Open this publication in new window or tab >>A New Library of Synthetic Spectra and Photometry for Evolved C Stars
2015 (English)In: WHY GALAXIES CARE ABOUT AGB STARS III: A CLOSER LOOK IN SPACE AND TIME, ASTRONOMICAL SOC PACIFIC , 2015, Vol. 497, p. 111-112Conference paper, Published paper (Refereed)
Abstract [en]

We present a library of synthetic spectra and photometry calculated on the basis of a grid of atmosphere and wind models for carbon-rich, pulsating AGB stars. The spectra cover the range between 0.35 and 25 mu m with a spectral resolution of R=200. The corresponding photometric variations during several pulsation periods were computed for standard broadband filters in the visual and near-infrared.

Place, publisher, year, edition, pages
ASTRONOMICAL SOC PACIFIC, 2015
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-294832 (URN)000371098100016 ()9781583818794 (ISBN)
Conference
Conference on Why Galaxies Care About AGB Stars III: A Closer Look in Space and Time, JUL 28-AUG 01, 2014, Univ Vienna, Vienna, AUSTRIA
Available from: 2016-08-18 Created: 2016-05-27 Last updated: 2016-08-18Bibliographically approved
Ryde, N., Lambert, J., Richter, M. J., Josselin, E., Harper, G. M., Eriksson, K., . . . Vacca, W. (2015). Evolved Stars with Complex Atmospheres - the High Spectral Resolution, mid-IR View. In: Why galaxies care about AGB stars III: a closer look in space and time. Paper presented at Conference on Why Galaxies Care About AGB Stars III: A Closer Look in Space and Time, JUL 28-AUG 01, 2014, Univ Vienna, Vienna, AUSTRIA (pp. 67-71). ASTRONOMICAL SOC PACIFIC, 497
Open this publication in new window or tab >>Evolved Stars with Complex Atmospheres - the High Spectral Resolution, mid-IR View
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2015 (English)In: Why galaxies care about AGB stars III: a closer look in space and time, ASTRONOMICAL SOC PACIFIC , 2015, Vol. 497, p. 67-71Conference paper, Published paper (Refereed)
Abstract [en]

The physical structures of the outer atmospheres of red giants are not known. They are certainly complex, and a range of recent observations are showing that we need to embrace non-classical model atmospheres to interpret these regions. This region's properties are of importance, not the least for an understanding of the mass-loss mechanism for these stars. Here we present observational constraints on the outer regions of red giants, based on mid-IR, high spectral resolution spectra. We also discuss possible non-LTE effects and highlight a new non-LTE code that will be used to analyse the spectra of these atmospheric layers. We conclude by mentioning our new SOFIA/EXES observations of red giants at 67 mu m, where the vibration-rotation lines of water vapour can be detected and spectrally resolved for the first time.

Place, publisher, year, edition, pages
ASTRONOMICAL SOC PACIFIC, 2015
Series
Astronomical Society of the Pacific conference series, ISSN 1050-3390 ; 497
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-301746 (URN)000371098100008 ()978-1-58381-879-4 (ISBN)978-1-58381-878-7 (ISBN)
Conference
Conference on Why Galaxies Care About AGB Stars III: A Closer Look in Space and Time, JUL 28-AUG 01, 2014, Univ Vienna, Vienna, AUSTRIA
Available from: 2016-08-24 Created: 2016-08-24 Last updated: 2016-08-24Bibliographically approved
Bladh, S., Höfner, S., Aringer, B. & Eriksson, K. (2015). Exploring Mass-Loss in M-type AGB Stars. In: WHY GALAXIES CARE ABOUT AGB STARS III: A CLOSER LOOK IN SPACE AND TIME. Paper presented at Conference on Why Galaxies Care About AGB Stars III: A Closer Look in Space and Time, JUL 28-AUG 01 2014, Univ Vienna, Vienna, AUSTRIA (pp. 345-350). ASTRONOMICAL SOC PACIFIC, 497
Open this publication in new window or tab >>Exploring Mass-Loss in M-type AGB Stars
2015 (English)In: WHY GALAXIES CARE ABOUT AGB STARS III: A CLOSER LOOK IN SPACE AND TIME, ASTRONOMICAL SOC PACIFIC , 2015, Vol. 497, p. 345-350Conference paper, Published paper (Refereed)
Abstract [en]

Stellar winds observed in asymptotic giant branch (AGB) stars are usually attributed to a combination of stellar pulsations and radiation pressure on dust. Strong candidates for wind-driving dust species in M-type AGB stars are magnesium silicates (Mg2SiO4 and MgSiO3). Such grains can form close to the stellar surface; they consist of abundant materials and, if they grow to sizes comparable to the wavelength of the stellar flux maximum, they experience strong acceleration by photon scattering. Here we present results from an extensive set of time-dependent wind models for M-type AGB stars with a detailed description for the growth of Mg2SiO4 grains. We show that these models reproduce observed mass-loss rates and wind velocities, as well as visual and near-IR photometry. However, the current models do not show the characteristic silicate features at 10 and 18 mu m, due to a rapidly falling temperature of Mg2SiO4 grains in the wind. Including a small amount of Fe in the grains further out in the circumstellar envelope will increase the grain temperature and result in pronounced silicate features, without significantly affecting the photometry in the visual and near-IR.

Place, publisher, year, edition, pages
ASTRONOMICAL SOC PACIFIC, 2015
National Category
Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-294842 (URN)000371098100068 ()
Conference
Conference on Why Galaxies Care About AGB Stars III: A Closer Look in Space and Time, JUL 28-AUG 01 2014, Univ Vienna, Vienna, AUSTRIA
Available from: 2016-05-27 Created: 2016-05-27 Last updated: 2016-05-27Bibliographically approved
Bladh, S., Susanne, H., Aringer, B. & Eriksson, K. (2015). Exploring wind-driving dust species in cool luminous giants III: Wind models for M-type AGB stars. Astronomy and Astrophysics, 575, Article ID A105.
Open this publication in new window or tab >>Exploring wind-driving dust species in cool luminous giants III: Wind models for M-type AGB stars
2015 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 575, article id A105Article in journal (Refereed) Published
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Astronomy
Identifiers
urn:nbn:se:uu:diva-230644 (URN)10.1051/0004-6361/201424917 (DOI)000360710400006 ()
Funder
Swedish Research Council
Available from: 2014-08-27 Created: 2014-08-27 Last updated: 2017-12-05Bibliographically approved
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