J/AJ/155/165 Dissipation in exoplanet hosts from tidal spin-up (Penev+, 2018)
Empirical tidal dissipation in exoplanet hosts from tidal spin-up.
Penev K., Bouma L.G., Winn J.N., Hartman J.D.
<Astron. J., 155, 165 (2018)>
=2018AJ....155..165P 2018AJ....155..165P (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Stars, masses ;
Stars, diameters ; Models
Keywords: planet-star interactions - planetary systems - stars: rotation
Abstract:
Stars with hot Jupiters (HJs) tend to rotate faster than other stars
of the same age and mass. This trend has been attributed to tidal
interactions between the star and planet. A constraint on the dissipation
parameter Q*' follows from the assumption that tides have managed to
spin up the star to the observed rate within the age of the system. This
technique was applied previously to HATS-18 and WASP-19. Here, we analyze
the sample of all 188 known HJs with an orbital period <3.5 days and a
"cool" host star (Teff<6100 K). We find evidence that the tidal
dissipation parameter (Q*') increases sharply with forcing frequency,
from 105 at 0.5 day-1 to 107 at 2 day-1. This helps to resolve
a number of apparent discrepancies between studies of tidal dissipation in
binary stars, HJs, and warm Jupiters. It may also allow for a HJ to damp
the obliquity of its host star prior to being destroyed by tidal decay.
Description:
We selected all of the known transiting planets from the NASA exoplanet
archive (http://exoplanetarchive.ipac.caltech.edu/) for which the planet
mass exceeds 0.1 MJup, the orbital period is shorter than 3.5 days,
and the star has an effective temperature below 6100 K. The effective
temperature cut-off ensures that only stars with surface convective zones
are included in the analysis. We decided to focus on these "cool" stars
because both theoretical expectations and observations suggest the
dominant tidal dissipation mechanism, and hence its efficiency, is
dramatically different for stars without a significant surface convective
zone. The restrictions on planet mass and orbital period were designed
to select systems with strong tides, for which the host stars are most
likely to have been measurably spun up. This resulted in an initial sample
of 188 systems.
Of the 188 systems in the sample, our procedure led to two-sided limits
on Q*' for 35 systems. In another 40 cases, it was possible to derive
a lower bound on Q*'. In the remaining cases, the data did not lead
to meaningful constraints. Table 1 summarizes the quantitative results
for each system.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 204 75 Derived stellar quality factors for all systems
with single or two-sided constraints
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See also:
J/ApJ/707/446 : HAT-P-13 photometry follow-up (Bakos+, 2009)
J/A+A/531/A24 : WASP-23 photometric and radial velocity data (Triaud+, 2011)
J/A+A/533/A88 : WASP-50b photometry and radial velocities (Gillon+, 2011)
J/ApJ/734/109 : Follow-up photometry of HAT-P-27 (Beky+, 2011)
J/ApJ/750/84 : Follow-up photometry and velocity of Qatar 2 (Bryan+, 2012)
J/ApJ/757/18 : Radial velocities for 16 hot Jupiter host stars
(Albrecht+, 2012)
J/A+A/558/A86 : HAT-P-42b and HAT-P-43b ri light curves (Boisse+, 2013)
J/A+A/559/A36 : Exoplanets WASP-65b and WASP-75b (Gomez Maqueo Chew+, 2013)
J/A+A/570/A64 : WASP-104b and WASP-106b photometry (Smith+, 2014)
J/AJ/148/29 : Spectroscopy and differential photometry of HATS-4
(Jordan+, 2014)
J/MNRAS/440/1982 : WASP 95-101 transits (Hellier+, 2014)
J/AJ/150/33 : Photometry and spectroscopy of HATS-9 and HATS-10
(Brahm+, 2015)
J/AJ/150/168 : Spectroscopy and photometry for HAT-P-50--HAT-P-53
(Hartman+, 2015)
J/A+A/586/A93 : WASP41 and WASP47 photometric and RV data
(Neveu-VanMalle+, 2016)
J/AJ/151/138 : Discovery of 2 hot Jupiters KELT-14b + KELT-15b
(Rodriguez+, 2016)
J/AJ/152/108 : i filter photometry for HATS-25 through HATS-30
(Espinoza+, 2016)
J/AJ/152/127 : Sloan i follow-up light curves of HATS-18 (Penev+, 2016)
J/AJ/152/182 : iz follow-up photometry of HAT-P-65 and HAT-P-66
(Hartman+, 2016)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- ID System identifier
12- 21 F10.8 d Per [0.78883899/3.4252602] Orbital period
23- 30 E8.2 d E_Per [4e-08/0.00016]? Upper uncertainty in Per
32- 39 E8.2 d e_Per [4e-08/0.00016]? Lower uncertainty in Per
41- 49 E9.3 d SPer [4.52/280] Spin period
51- 58 E8.2 d E_SPer [0.002/567] Upper uncertainty in SPer
60- 67 E8.2 d e_SPer [0.002/567] Lower uncertainty in SPer
69- 77 E9.3 Msun M* [0.58/1.29] Stellar mass
79- 86 E8.2 Msun E_M* [0.01/0.15] Upper uncertainty in M*
88- 95 E8.2 Msun e_M* [0.01/0.15] Lower uncertainty in M*
97-105 E9.3 Rsun R* [0.55/1.86] Stellar radius
107-114 E8.2 Rsun E_R* [0.01/0.14] Upper uncertainty in R*
116-123 E8.2 Rsun e_R* [0.01/0.13] Lower uncertainty in R*
125-133 E9.3 Mjup Mp [0.378/7.246] Planetary mass
135-142 E8.2 Mjup E_Mp [0.013/0.38] Upper uncertainty in Mp
144-151 E8.2 Mjup e_Mp [0.013/0.38] Lower uncertainty in Mp
153-161 E9.3 Rjup Rp [0.683/1.89] Planetary radius
163-170 E8.2 Rjup E_Rp [0.013/0.42] Upper uncertainty in Rp
172-179 E8.2 Rjup e_Rp [0.013/0.4] Lower uncertainty in Rp
181-181 A1 --- l_logQ [>] Limit flag on logQ
182-186 F5.3 [-] logQ [3.3/7.603] Log of the dissipation parameter
log10(Q*')
188-195 E8.2 [-] E_logQ [0.0491/3.07]? Upper uncertainty in logQ
197-204 E8.2 [-] e_logQ [0.0472/1.46]? Lower uncertainty in logQ
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 19-Nov-2018