2015ApJ...812..112S


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.24CET09:42:35

2015ApJ...812..112S - Astrophys. J., 812, 112 (2015/October-3)

The K2-ESPRINT project I: discovery of the disintegrating rocky planet K2-22b with a cometary head and leading tail.

SANCHIS-OJEDA R., RAPPAPORT S., PALLE E., DELREZ L., DEVORE J., GANDOLFI D., FUKUI A., RIBAS I., STASSUN K.G., ALBRECHT S., DAI F., GAIDOS E., GILLON M., HIRANO T., HOLMAN M., HOWARD A.W., ISAACSON H., JEHIN E., KUZUHARA M., MANN A.W., MARCY G.W., MILES-PAEZ P.A., MONTANES-RODRIGUEZ P., MURGAS F., NARITA N., NOWAK G., ONITSUKA M., PAEGERT M., VAN EYLEN V., WINN J.N. and YU L.

Abstract (from CDS):

We present the discovery of a transiting exoplanet candidate in the K2 Field-1 with an orbital period of 9.1457 hr: K2-22b. The highly variable transit depths, ranging from ∼0% to 1.3%, are suggestive of a planet that is disintegrating via the emission of dusty effluents. We characterize the host star as an M-dwarf with Teff~= 3800 K. We have obtained ground-based transit measurements with several 1-m class telescopes and with the GTC. These observations (1) improve the transit ephemeris; (2) confirm the variable nature of the transit depths; (3) indicate variations in the transit shapes; and (4) demonstrate clearly that at least on one occasion the transit depths were significantly wavelength dependent. The latter three effects tend to indicate extinction of starlight by dust rather than by any combination of solid bodies. The K2 observations yield a folded light curve with lower time resolution but with substantially better statistical precision compared with the ground-based observations. We detect a significant ''bump'' just after the transit egress, and a less significant bump just prior to transit ingress. We interpret these bumps in the context of a planet that is not only likely streaming a dust tail behind it, but also has a more prominent leading dust trail that precedes it. This effect is modeled in terms of dust grains that can escape to beyond the planet's Hill sphere and effectively undergo ''Roche lobe overflow,'' even though the planet's surface is likely underfilling its Roche lobe by a factor of 2.

Abstract Copyright:

Journal keyword(s): planetary systems - planets and satellites: atmospheres - planets and satellites: detection

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2605 0
2 NGC 2632 OpC 08 40 24 +19 40.0           ~ 1191 0
3 K2-22 LM* 11 17 55.8771414480 +02 37 08.603887613   17.04 15.60 15.38   K7V 22 0
4 K2-22b Pl 11 17 55.8771414480 +02 37 08.603887613           ~ 35 0
5 K2-3 PM* 11 29 20.3917940095 -01 27 17.279810476   13.52 12.17 11.88   M0.0V 45 0
6 K2-19 * 11 39 50.4804464997 +00 36 12.877309991   13.80 13.00 12.88   ~ 28 0
7 EPIC 201918073 * 11 49 04.9703196076 +07 42 37.693294696           ~ 1 0
8 KOI-72.01 Pl 19 02 43.0612302512 +50 14 28.700759378           ~ 229 1
9 NAME KIC 12557548b Pl? 19 23 51.8899069766 +51 30 16.983558676           ~ 56 1
10 NAME KIC 8435766b Pl 19 34 58.0139307295 +44 26 53.957326851           ~ 99 1
11 KOI-2700b Pl? 19 48 00.8488827355 +44 46 30.374871297           ~ 28 0
12 KOI-2700 Ro* 19 48 00.8488827355 +44 46 30.374871297           ~ 27 0
13 BD-00 4534 PM* 23 35 49.2850796143 +00 26 43.842763271   11.10   9.6   K0 36 0

    Equat.    Gal    SGal    Ecl

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2020.01.24-09:42:35

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