Thomas R. Geballe
University of Hawaii at Manoa
312 Papers
4.5K Citations
Thomas R. Geballe is an academic researcher from University of Hawaii at Manoa. The author has contributed to research in topics: Stars & Brown dwarf. The author has an hindex of 71, co-authored 301 publications.
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Papers
3.6-7.9 μm Photometry of L and T Dwarfs and the Prevalence of Vertical Mixing in their Atmospheres
S. K. Leggett,Didier Saumon,Mark S. Marley,Thomas R. Geballe,David A. Golimowski,Denise C. Stephens,Xiaohui Fan +6 more
TL;DR: In this article, the authors explored the effect of gravity and metallicity on the mid-infrared colors of L and T dwarfs and found that the data are modeled satisfactorily only if substantial vertical mixing occurs in both L andT dwarf atmospheres.
The continuing saga of Sakurai's object (V4334 Sgr): dust production and helium line emission
V. H. Tyne,S. P. S. Eyres,Thomas R. Geballe,A. Evans,Barry Smalley,Hilmar W. Duerbeck,Martin Asplund +6 more
TL;DR: In this paper, the authors conclude that the excitation is collisional and is probably caused by a wind, consistent with the P Cygni profile observed by Eyres et al. in 1998.
Analysis of the 3.2–3.3 μm Interstellar Absorption Feature on Three Milky Way Sightlines
L. S. Bernstein,Thomas R. Geballe +1 more
TL;DR: Analysis of the 3.2–3.3 μm Interstellar Absorption Feature on Three Milky Way Sightlines finds that the 3.2–3.3 μm absorption feature is well fit by a superposition of four Gaussians, with the shortest-wavelength Gaussian being associated with irregularly shaped PAHs.
Search for H3+ in HD141569A
Miwa Goto,Thomas R. Geballe,Benjamin J. McCall,Tomonori Usuda,Hiroshi Suto,Hiroshi Terada,Naoto Kobayashi,Takeshi Oka +7 more
TL;DR: In this paper, a search for H3+ line emission, reported to have been detected toward the young star HD 141569A and possibly originating in a clump of planet-forming gas orbiting the star, has yielded negative results.
Detection of Water Ice on Saturn's Satellite Phoebe
TL;DR: In this article, the surface of Phoebe was modeled with an intimate (granular) mix of H2O ice (3% by weight, grain size 500 micrometers) mixed with fine grains of H 2O ice with amorphous carbon (grain size 900 micrometer) as the dominant component.