Circumstellar Shells of A-K Luminous Supergiants

Hinkle, Kenneth H.

doi:10.1007/978-94-009-3887-8_80

Cited by 4 publications

(5 citation statements)

References 7 publications

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“…Phoenix is a highresolution λ/Δλ = 50,000 (4 pixel slit − 0″.34), near-infrared 1 -5 µm spectrometer. An individual spectrum is single order and covers a very narrow wavelength range of 0.5% of the central wavelength, corresponding to a radial velocity range of 1500 km/sec (Hinkle et al 1998;Hinkle et al 2000;Hinkle et al 2003). We observed HD 100453 with one M-band setting centered at 4.97 µm.…”

Section: Gemini South Phoenix Echelle Spectroscopymentioning

confidence: 75%

Hd 100453: A Link Between Gas-Rich Protoplanetary Disks and Gas-Poor Debris Disks

Collins

Grady

Hamaguchi

et al. 2009

ApJ

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HD 100453 has an IR spectral energy distribution (SED) which can be fit with a power-law plus a blackbody. Previous analysis of the SED suggests that the system is a young Herbig Ae star with a gas-rich, flared disk. We reexamine the evolutionary state of the HD 100453 system by refining its age (based on a candidate low-mass companion) and by examining limits on the disk extent, mass accretion rate, and gas content of the disk environment. We confirm that HD 100453B is a common proper motion companion to HD 100453A, with a spectral type of M4.0V − M4.5V, and derive an age of 10 ± 2 Myr. We find no evidence of mass accretion onto the star. Chandra ACIS-S imagery shows that the Herbig Ae star has L x /L bol and an X-ray spectrum similar to non-accreting β Pic Moving Group early F stars. Moreover, the disk lacks the conspicuous Fe II emission and excess FUV continuum seen in spectra of actively accreting Herbig Ae stars, and from the FUV continuum, we find the accretion rate is < 1.4×10 −9 M  yr −1 . A sensitive upper limit to the CO J = 3−2 intensity indicates that the gas in the outer disk is likely optically thin. Assuming a [CO]/[H 2 ] abundance of 1×10 −4 and a depletion factor of 10 3 , we find that the mass of cold molecular gas is less than ~0.33 M J and that the gas-to-dust ratio is no more than ~4:1 in the outer disk. The combination of a high fractional IR excess luminosity, a relatively old age, an absence of accretion signatures, and an absence of detectable circumstellar molecular gas suggests that the HD 100453 system is in an unusual state of evolution between a gas-rich protoplanetary disk and a gas-poor debris disk.

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Section: Gemini South Phoenix Echelle Spectroscopymentioning

confidence: 75%

Hd 100453: A Link Between Gas-Rich Protoplanetary Disks and Gas-Poor Debris Disks

Collins

Grady

Hamaguchi

et al. 2009

ApJ

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“…If triatomic H 2 O is responsible for this line, then it should be much weaker in giant stars of similar effective temperature, and this can be seen in the spectal atlas of Arcturus (Hinkle, Wallace, & Livingston 1995); although having a similar effective temperature to JW163 or JW433, this feature is not detectable in Arcturus, even though the HF line is clearly visible. Indeed, a tentative identification has been provided by Hinkle (2004) as H 2 O (021) [14,5,9]-(010) [13,11,2] at an air wavelength of about 23356.4Å.…”

Section: Fluorine Carbon and Oxygen Abundancesmentioning

confidence: 99%

Fluorine Abundances in the Orion Nebula Cluster

Cunha

Smith

2005

ApJ

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This study uses cool dwarfs as sources with which to probe fluorine abundances via HF. This molecule is detected for the first time in young K-M dwarf members of an OB association. Fluorine, oxygen, and carbon abundances were derived from the HF(1--0) R9 line along with samples of OH and CO vibration-rotation lines present in high-resolution infrared spectra observed with the Phoenix spectrograph on the Gemini South Telescope. The fluorine and oxygen results obtained for these targets, still in the pre-main-sequence stage of evolution, agree well with the general trend defined for the Milky Way disk; the latter being deduced from observations of more evolved giant stars. In addition, the carbon and oxygen abundances obtained for the studied stars overlap results from previous studies of the more massive OB stars and FG dwarf members of the Orion Nebula Cluster. We conclude from this agreement that the fluorine abundances derived for the Orion K-M dwarfs (when there is no conspicuous evidence of disks) can be considered a good representation of the current fluorine abundance value for the Milky Way disk.Comment: 18 pages, including 2 tables and 3 figures. Accepted for publication in The Astrophysical Journa

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“…Phoenix is a high-resolution / = 50,000 (4 pixel slit -0 .34), near-infrared 1 -5 μm spectrometer. An individual spectrum is single order and covers a very narrow wavelength range of 0.5% of the central wavelength, corresponding to a radial velocity range of 1500 km/sec (Hinkle et al 1998;Hinkle et al 2000;Hinkle et al 2003). We observed HD 100453 with one M-band setting centered at 4.97 μm.…”

Section: Gemini South Phoenix Echelle Spectroscopymentioning

confidence: 73%

HD 100453: An Evolutionary Link Between Protoplanetary Disks and Debris Disks

Collins¹,

Grady²,

Hamaguchi³

et al. 2009

AIP Conference Proceedings

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provided common proper motion data reduction from the VLT NACO observations. Bruce Woodgate of NASA/GSFC and Thomas Henning of the Max-Planck-Institut für Astronomie provided overall scientific support, detailed comments, and direction. George Hartig of STScI contributed information regarding the SBC design and investigated the probable source of the SBC optical ghost.Herbig Ae stars are young stars usually surrounded by gas and dust in the form of a disk and are thought to evolve into planetary systems similar to our own. We present a multi-wavelength examination of the disk and environment of the Herbig Ae star HD 100453A, focusing on the determination of accretion rate, system age, and disk evolution. We show that the accretion rate is characterized by Chandra X-ray imagery that is inconsistent with strongly accreting early F stars, that the disk lacks the conspicuous Fe II emission and continuum seen in FUV spectra of actively accreting Herbig Ae stars, and that FUSE, HST, and FEROS data suggest an accretion rate below ~2.5 10 10 M yr 1 . We confirm that HD 100453B is a common proper motion companion to HD 100453A, with spectral type M4.0V M4.5V, and derive an age of 14 ± 4 Myr. We examine the Meeus et al. (2001) hypothesis that Meeus Group I sources, which have a mid-IR bump which can be fitted by a black body component, evolve to Meeus Group II sources, which have no such mid-IR bump. By considering stellar age and accretion rate evidence, we find the hypothesis to be invalid. Furthermore, we find that the disk characteristics of HD 100453A do not fit the traditional definition of a protoplanetary disk, a transitional disk, or a debris disk, and they may suggest a new class of disks linking gas-rich protoplanetary disks and gas-poor debris disks.vii

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Circumstellar Shells of A-K Luminous Supergiants

Cited by 4 publications

References 7 publications

Hd 100453: A Link Between Gas-Rich Protoplanetary Disks and Gas-Poor Debris Disks

Hd 100453: A Link Between Gas-Rich Protoplanetary Disks and Gas-Poor Debris Disks

Fluorine Abundances in the Orion Nebula Cluster

HD 100453: An Evolutionary Link Between Protoplanetary Disks and Debris Disks

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