Planet KOI-74 b

Detailed information about planet KOI-74 b and its parameters.

Planet parameters Publications Observability Predictor

Planet

Name

KOI-74 b

Planet Status

Candidate

Discovered in

2010

Update

2021-10-02

Mass

264.0 (\begin{matrix} + 26.0 \\ - 26.0 \end{matrix})

M_J 1 publication

SOPHIE velocimetry of Kepler transit candidates. I. Detection of the low-mass white dwarf KOI-74b

Mass*sin(i)

—

Semi-Major Axis

0.074 AU 1 publication

Kepler Observations of Transiting Hot Compact Objects

Orbital Period

5.188754 (\pm 8.3e-05)

day 1 publication

Kepler Observations of Transiting Hot Compact Objects

Eccentricity

— 1 publication

Kepler Observations of Transiting Hot Compact Objects

ω

—

T_peri

— 1 publication

Kepler Observations of Transiting Hot Compact Objects

Radius

0.4 (\begin{matrix} + 0.02 \\ - 0.02 \end{matrix})

R_J 1 publication

Kepler Observations of Transiting Hot Compact Objects

Inclination

88.8 (\pm 0.5)

deg 1 publication

Kepler Observations of Transiting Hot Compact Objects

Detection Method

Other

Mass Meas. Method

—

Radius Meas. Method

—

Primary transit

2454958.87995 (\pm 0.00036)

Secondary transit

—

λ

—

Impact Parameter b

—

Time V_r=0

—

Velocity Semiamplitude K

—

Calculated temperature

—

Measured temperature

—

Hottest point longitude

—

Geometric albedo

—

Surface gravity log(g/g_H)

—

Alternate Names

—

Data Source	Type	Result Value	Result Figure	Notes	Reference

Molecule	Data Source	Type	Result Value	Result Figure	Notes	Reference

13 Sep. 2010: This objected was initially attributed a 19 MJup mass (Rowe et al. 2010). But subsequent RV measuremnts lead to a 0.252 solar mass, making it a white dwarf (Ehrenreich et al. 2010).
22 Jan. 2009: The detection of the object, detected by transit (Rowe et al. 2009) is undoubtfull. But what makes its planetary nature problematic is its very high measured temperature: 1289 +/- 340 K. If it were only heated by its parent star, its expected equilibrium temperature would be 2250 +/- 50 K at most (Rowe et al. 2009).
Note that the mass is not derived from RV measurements of the parent star, but from the ratio of the tidal acceleration to the star's surface gravity (Rowe et al. 2009).

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