Planet GJ 96 b

Detailed information about planet GJ 96 b and its parameters.

Planet parameters Publications Observability Predictor

Planet

Name

GJ 96 b

Planet Status

Retracted

Discovered in

2018

Update

2024-08-04

Mass

0.06186 (\begin{matrix} + 0.00761 \\ - 0.0072 \end{matrix})

M_J

Mass*sin(i)

0.06186 (\begin{matrix} + 0.00761 \\ - 0.0072 \end{matrix})

M_J 1 publication

The SOPHIE search for northern extrasolar planets. XIII. Two planets around M-dwarfs Gl617A and Gl96

Semi-Major Axis

0.291 (\pm 0.005)

AU 1 publication

The SOPHIE search for northern extrasolar planets. XIII. Two planets around M-dwarfs Gl617A and Gl96

Orbital Period

73.94 (\begin{matrix} + 0.33 \\ - 0.38 \end{matrix})

day 1 publication

The SOPHIE search for northern extrasolar planets. XIII. Two planets around M-dwarfs Gl617A and Gl96

Eccentricity

0.44 (\begin{matrix} + 0.11 \\ - 0.09 \end{matrix})

1 publication

The SOPHIE search for northern extrasolar planets. XIII. Two planets around M-dwarfs Gl617A and Gl96

ω

339.58 (\begin{matrix} + 12.45 \\ - 14.52 \end{matrix})

deg 1 publication

The SOPHIE search for northern extrasolar planets. XIII. Two planets around M-dwarfs Gl617A and Gl96

T_peri

2455556.39 (\begin{matrix} + 10.57 \\ - 8.98 \end{matrix})

JD 1 publication

The SOPHIE search for northern extrasolar planets. XIII. Two planets around M-dwarfs Gl617A and Gl96

Radius

—

Inclination

—

Detection Method

Radial Velocity

Mass Meas. Method

Radial Velocity

Radius Meas. Method

—

Primary transit

—

Secondary transit

—

λ

—

Impact Parameter b

—

Time V_r=0

—

Velocity Semiamplitude K

4.69 (\begin{matrix} + 0.72 \\ - 0.62 \end{matrix})

m/s

Calculated temperature

—

Measured temperature

—

Hottest point longitude

—

Geometric albedo

—

Surface gravity log(g/g_H)

—

Alternate Names

GL96 b

Data Source	Type	Result Value	Result Figure	Notes	Reference

Molecule	Data Source	Type	Result Value	Result Figure	Notes	Reference

Ribas et al. (2023): The 75-day signal present in SOPHIE data is absent in the 53 RVs from CARMENES. Instead, the dominant signal is at 28.5 d, which Hobson et al. (2018) already attributed to stellar activity. Indeed, this period is also present in the dLW, Ca ii IRT, and Hα time series of the CARMENES data, thus ruling out its planetary nature.

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