| タイトル | A Combined Very Large Telescope and Gemini Study of the Atmosphere of the Directly Imaged Planet, Beta Pictoris b |
| 本文（外部サイト） | http://hdl.handle.net/2060/20140005673 |
| 著者（英） | Murray-Clay, Ruth; Burrows, Adam; Fukagawa, Misato; Dawson, Rebekah; Girard, Julien H.; Madhusudhan, Nikku; Jayawardhana, Ray; Kuchner, Marc J.; Bromley, Ben; Kenyon, Scott; Currie, Thayne; Chambers, John; Matsumura, Soko |
| 著者所属（英） | NASA Goddard Space Flight Center |
| 発行日 | 2013-10-10 |
| 言語 | eng |
| 内容記述 | We analyze new/archival VLT/NaCo and Gemini/NICI high-contrast imaging of the young, self-luminous planet Beta Pictoris b in seven near-to-mid IR photometric filters, using advanced image processing methods to achieve high signal-to-noise, high precision measurements. While Beta Pic b's near-IR colors mimic those of a standard, cloudy early-to-mid L dwarf, it is overluminous in the mid-infrared compared to the field L/T dwarf sequence. Few substellar/planet-mass objects-i.e., And b and 1RXJ 1609B-match Beta Pic b's JHKsL photometry and its 3.1 micron and 5 micron photometry are particularly difficult to reproduce. Atmosphere models adopting cloud prescriptions and large (approx. 60 micron)dust grains fail to reproduce the Beta Pic b spectrum. However, models incorporating thick clouds similar to those found forHR8799 bcde, but also with small (a fewmicrons) modal particle sizes, yield fits consistent with the data within the uncertainties. Assuming solar abundance models, thick clouds, and small dust particles (a = 4 micron), we derive atmosphere parameters of log(g) = 3.8 +/- 0.2 and Teff = 1575-1650 K, an inferred mass of 7+4 3 MJ, and a luminosity of log(L/L) approx. 3.80 +/- 0.02. The best-estimated planet radius, is approx. equal to 1.65 +/- 0.06 RJ, is near the upper end of allowable planet radii for hot-start models given the host star's age and likely reflects challenges constructing accurate atmospheric models. Alternatively, these radii are comfortably consistent with hot-start model predictions if Beta Pic b is younger than is approx. equal to 7 Myr, consistent with a late formation well after its host star's birth approx. 12+8 4 Myr ago. |
| NASA分類 | Astrophysics |
| レポートNO | GSFC-E-DAA-TN12649 |
| 権利 | Copyright, Distribution as joint owner in the copyright |
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