Royer, P; Decin, L; Wesson, R; Barlow, MJ; Polehampton, ET; Matsuura, M; ... Yates, JA; + view all Royer, P; Decin, L; Wesson, R; Barlow, MJ; Polehampton, ET; Matsuura, M; Agundez, M; Blommaert, JADL; Cernicharo, J; Cohen, M; Daniel, F; Degroote, P; De Meester, W; Exter, K; Feuchtgruber, H; Gear, WK; Gomez, HL; Groenewegen, MAT; Hargrave, PC; Huygen, R; Imhof, P; Ivison, RJ; Jean, C; Kerschbaum, F; Leeks, SJ; Lim, T; Lombaert, R; Olofsson, G; Posch, T; Regibo, S; Savini, G; Sibthorpe, B; Swinyard, BM; Vandenbussche, B; Waelkens, C; Witherick, DK; Yates, JA; - view fewer (2010) PACS and SPIRE spectroscopy of the red supergiant VY CMa. ASTRON ASTROPHYS , 518 , Article L145. 10.1051/0004-6361/201014641.
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With a luminosity > 10(5) L-circle dot and a mass-loss rate of similar to 2 x 10(-4) M-circle dot yr(-1), the red supergiant VY CMa truly is a spectacular object. Because of its extreme evolutionary state, it could explode as supernova any time. Studying its circumstellar material, into which the supernova blast will run, provides interesting constraints on supernova explosions and on the rich chemistry taking place in such complex circumstellar envelopes. We have obtained spectroscopy of VY CMa over the full wavelength range offered by the PACS and SPIRE instruments of Herschel, i.e. 55-672 micron. The observations show the spectral fingerprints of more than 900 spectral lines, of which more than half belong to water. In total, we have identified 13 different molecules and some of their isotopologues. A first analysis shows that water is abundantly present, with an ortho-to-para ratio as low as similar to 1.3:1, and that chemical non-equilibrium processes determine the abundance fractions in the inner envelope.
|Title:||PACS and SPIRE spectroscopy of the red supergiant VY CMa|
|Keywords:||line: identification, stars: chemically peculiar, circumstellar matter, stars: mass-loss, supergiants, RICH EVOLVED STARS, CANIS-MAJORIS, WATER-VAPOR, IK TAURI, EMISSION, SPECTRUM, CARBON, CHEMISTRY, ENVELOPE, VYCMA|
|UCL classification:||UCL > School of BEAMS > Faculty of Maths and Physical Sciences > Physics and Astronomy|
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