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The PTF Orion Project: a Possible Planet Transiting a T-Tauri Star | | Julian C. van Eyken
; David R. Ciardi
; Kaspar von Braun
; Stephen R. Kane
; Peter Plavchan
; Chad F. Bender
; Timothy M. Brown
; Justin Crepp
; Benjamin J. Fulton
; Andrew W. Howard
; Steve B. Howell
; Suvrath Mahadevan
; Geoffrey W. Marcy
; Avi Shporer
; Paula Szkody
; Rachel L. Akeson
; Charles A. Beichman
; Andrew F. Boden
; Dawn M. Gelino
; D. W. Hoard
; Solange V. Ramírez
; Luisa M. Rebull
; John R. Stauffer
; Joshua S. Bloom
; S. Bradley Cenko
; Mansi M. Kasliwal
; Shrinivas R. Kulkarni
; Nicholas M. Law
; Peter E. Nugent
; Eran O. Ofek
; Dovi Poznanski
; Robert M. Quimby
; Richard Walters
; Carl J. Grillmair
; Russ Laher
; David B. Levitan
; Branimir Sesar
; Jason A. Surace
; | | Date: |
7 Jun 2012 | | Abstract: | We report observations of a possible young transiting planet orbiting a
previously known weak-lined T-Tauri star in the 7-10Myr-old Orion-OB1a/25-Ori
region. The candidate was found as part of the Palomar Transient Factory (PTF)
Orion project. It has a photometric transit period of 0.448413 pm 0.000040
days, and appears in both 2009 and 2010 PTF data. Follow-up low-precision
radial velocity observations and adaptive-optics imaging suggest that the star
is not an eclipsing binary, and that it is unlikely that a background source is
blended with the target and mimicking the observed transit. Radial-velocity
observations with the Hobby-Eberly and Keck telescopes yield a radial velocity
that has the same period as the photometric event, but is offset in phase from
the transit center by approx -0.22 periods. The amplitude (half range) of the
radial velocity variations is 2.4 km/s and is comparable with the expected
radial velocity amplitude that stellar spots could induce. The radial velocity
curve is likely dominated by stellar spot modulation and provides an upper
limit to the projected companion mass of Mp sin iorb leq 4.8pm1.2 MJup; when
combined with the orbital inclination, iorb, of the candidate planet from
modeling of the transit lightcurve, we find an upper limit on the mass of the
planetary candidate of Mp leq 5.5pm1.4 MJup. This limit implies that the
planet is orbiting close to, if not inside, its Roche limiting orbital radius,
so that it may be undergoing active mass loss and evaporating. | | Source: | arXiv, 1206.1510 | | Services: | Forum | Review | PDF | Favorites | |
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