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%.

alpha-orionis

stars

circumstellar envelopes

nebulae

AGB and post-AGB

submillimeter

afgl-2343

giant branch stars

rotational line-profiles

protoplanetary

emission

supergiants

evolved

circumstellar matter

mass-loss history

nml-cygni

Författare

D. Teyssier

European Space Astronomy Centre

G. Quintana-Lacaci

CSIC-INTA - Centro de Astrobiologia (CAB)

Instituto de Radioastronomia Milimetrica

A. P. Marston

European Space Astronomy Centre

V. Bujarrabal

Observatorio Astronomico Nacional

J. Alcolea

Observatorio Astronomico Nacional

J. Cernicharo

CSIC-INTA - 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

Sterrekundig Instituut Utrecht

Universiteit Van Amsterdam

G. J. Melnick

Harvard-Smithsonian Center for Astrophysics

K. M. Menten

Max Planck-institutet

D. A. Neufeld

Johns Hopkins University

Hans Olofsson

Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium

P. Planesas

Observatorio Astronomico Nacional

M. Schmidt

Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences

R. Soria-Ruiz

Observatorio Astronomico Nacional

Fredrik Schöier

Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium

R. Szczerba

Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences

Lbfm Waters

Universiteit Van Amsterdam

SRON Netherlands Institute for Space Research

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 545 A99 (article no.)- A99

Ämneskategorier

Astronomi, astrofysik och kosmologi

DOI

10.1051/0004-6361/201219545