Herschel/HIFI observations of red supergiants and yellow hypergiants I. Molecular inventory
Artikel i vetenskaplig tidskrift, 2012
Context. Red supergiant stars (RSGs) and yellow hypergiant stars (YHGs) are believed to be the high-mass counterparts of stars in the asymptotic giant branch (AGB) and early post-AGB phases. As such, they are scarcer and the properties and evolution of their envelopes are still poorly understood. Aims. We study the mass-loss in the post main-sequence evolution of massive stars, through the properties of their envelopes in the intermediate and warm gas layers. These are the regions where the acceleration of the gas takes place and the most recent mass-loss episodes can be seen. Methods. We used the HIFI instrument on-board the Herschel Space Observatory to observe sub-millimetre and far-infrared (FIR) transitions of CO, water, and their isotopologues in a sample of two RSGs (NML Cyg and Betelgeuse) and two YHGs (IRC + 10420 and AFGL 2343) stars. We present an inventory of the detected lines and analyse the information revealed by their spectral profiles. A comparison of the line intensity and shape in various transitions is used to qualitatively derive a picture of the envelope physical structure. On the basis of the results presented in an earlier study, we model the CO and (CO)-C-13 emission in IRC + 10420 and compare it to a set of lines ranging from the millimetre to the FIR. Results. Red supergiants have stronger high-excitation lines than the YHGs, indicating that they harbour dense and hot inner shells contributing to these transitions. Consequently, these high-J lines in RSGs originate from acceleration layers that have not yet reached the circumstellar terminal velocity and have narrower profiles than their flat-topped lower-J counterparts. The YHGs tend to lack this inner component, in line with the picture of detached, hollow envelopes derived from studies at longer wavelengths. NH3 is only detected in two sources (NML Cyg and IRC + 10420), which are also observed to be the strongest water-line emitters of the studied sample. In contrast, OH is detected in all sources and does not seem to correlate with the water line intensities. We show that the IRC + 10420 model derived solely from millimetre low-J CO transitions is capable of reproducing the high-J transitions when the temperature in the inner shell is simply lowered by about 30%.
submillimeter
supergiants
emission
circumstellar envelopes
protoplanetary
rotational line-profiles
nebulae
mass-loss history
evolved
stars
afgl-2343
circumstellar matter
alpha-orionis
nml-cygni
giant branch stars
AGB and post-AGB
Författare
D. Teyssier
Europeiska rymdorganisationen (ESA)
G. Quintana-Lacaci
Centro de Astrobiologia (CAB)
Institut de Radioastronomie Millimétrique (IRAM)
A. P. Marston
Europeiska rymdorganisationen (ESA)
V. Bujarrabal
Observatorio Astronómico Nacional (OAN)
J. Alcolea
Observatorio Astronómico Nacional (OAN)
J. Cernicharo
Centro de Astrobiologia (CAB)
L. Decin
Universiteit Van Amsterdam
KU Leuven
C. Dominik
Universiteit Van Amsterdam
Radboud Universiteit
Kay Justtanont
Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium
A. de Koter
Universiteit Van Amsterdam
Universiteit Utrecht
G. J. Melnick
Harvard-Smithsonian Center for Astrophysics
K. M. Menten
Max-Planck-Gesellschaft
D. A. Neufeld
Johns Hopkins University
Hans Olofsson
Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium
P. Planesas
Observatorio Astronómico Nacional (OAN)
M. Schmidt
Polish Academy of Sciences
R. Soria-Ruiz
Observatorio Astronómico Nacional (OAN)
Fredrik Schöier
Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium
R. Szczerba
Polish Academy of Sciences
Lbfm Waters
Netherlands Institute for Space Research (SRON)
Universiteit Van Amsterdam
Astronomy and Astrophysics
0004-6361 (ISSN) 1432-0746 (eISSN)
Vol. 545 A99 (article no.)- A99Ämneskategorier (SSIF 2011)
Astronomi, astrofysik och kosmologi
DOI
10.1051/0004-6361/201219545