TEPCat: Kepler-35


 

This page summarises the information held within TEPCat for the transiting planetary system Kepler-35. Please see here for descriptions of the quantities given below.

This object consists of an eclipsing binary star system which is itself eclipsed by one or more transiting planets. The binarity of the central star causes problems for structured databases. The stellar data below refer specifically to the primary star, and the planetary data to the transiting planet. For further information on the secondary star or the system as a whole please consult the publication(s) referenced below.

 

Discovery and basic observable quantities:
 
Quantity Value Unit
Reference of discovery paper 2012Natur.481..475W  
Date of discovery paper 2012 / 1 / 26 y / m / d
Right ascension 19 37 59.28 h m s
Declination +46 41 23.1 d m s
V-band apparent magnitude 15.93 mag
K-band apparent magnitude 13.88 mag
Transit duration 0.4
( 10. )
day
hour
Transit depth 0.4 %
Time of mid-transit   2454965.85000 ± 0.0     HJD or BJD
Orbital period 131.458 ± 0.091 days
Reference for orbital ephemeris   2012Natur.481..475W  

 

Physical properties from the most recent detailed study:
 
Quantity Value Unit
Stellar effective temperature 5606 ± 150 K
Stellar metal abundance ([Fe/H] or [M/H])   −0.34 ± 0.20 dex
Stellar mass 0.8877 +0.0051 −0.0053   Msun
Stellar radius 1.0284 +0.0020 −0.0019 Rsun
Stellar logarithmic surface gravity 4.3623 ± 0.0020 c.g.s.
Stellar mean density ρsun
g cm-3
Orbital eccentricity 0.042 +0.007 −0.004  
Orbital semimajor axis   0.60347 +0.00101 −0.00103  AU
Planetary mass 0.127 ± 0.020
( 40.4 ± 6.4 )
Mjup
Mearth
Planetary radius 0.728 ± 0.014
( 8.16 ± 0.16 )
Rjup
Rearth
Planetary surface gravity 5.96 ± 0.98
2.78 ± 0.07
m/s2
log(cgs)
Planetary mean density 0.309 +0.053 −0.052
( 0.410 +0.070 −0.069 )
ρjup
g cm-3
Planetary equilibrium temperature K
Reference of detailed study 2012Natur.481..475W  

 

Kepler-35 does not have an entry in the catalogue of Rossiter-McLaughlin measurements.

 

Kepler-35 has not been analysed as part of the Homogeneous Studies of Transiting Extrasolar Planets project.

 


Page generated on 2017/12/12           John Southworth   (Keele University, UK)