Planet LHS 1140 c

Name LHS 1140 c
Planet Status Confirmed
Discovered in 2018
Mass 0.00569 (± 0.00123) MJ
Mass*sin(i)
Semi-Major Axis 0.02675 (± 0.0007) AU
Orbital Period 3.777931 (± 3e-06) day
Eccentricity 0.31 ( -0.31 +0.0 )
ω
Tperi
Radius 0.11437 (± 0.00214) RJ
Inclination 89.92 ( -0.09 +0.06 ) deg
Update 2020-05-09
Detection Method Primary Transit
Mass Detection Method Radial Velocity
Radius Detection Method Primary Transit
Primary transit 2458226.84317 (± 2.6e-05) JD
Secondary transit
λ
Impact Parameter b
Time Vr=0
Velocity Semiamplitude K 2.35 (± 0.49) m/s
Calculated temperature
Measured temperature
Hottest point longitude
Geometric albedo
Surface gravity log(g/gH)
Alternate Names

Star

LHS 1140
Name LHS 1140
Distance 12.47 (± 0.42) pc
Spectral type M4.5
Apparent magnitude V 14.15
Mass 0.146 (± 0.019) MSun
Age 5.0 ( -0.0 +8.0 ) Gyr
Effective temperature 3131.0 (± 100.0) K
Radius 0.186 (± 0.013) RSun
Metallicity [Fe/H] -0.24 (± 0.1)
Detected Disc
Magnetic Field
RA2000 00:44:59.0
Dec2000 -15:16:17
Alternate Names
Planetary system
2 planets

More data


Related publications

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A hot terrestrial planet orbiting the bright M dwarf L 168-9 unveiled by TESS
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Tidal evolution of exoplanetary systems hosting potentially habitable exoplanets. The cases of LHS-1140 b-c and K2-18 b-c
2020 GOMES G. & FERRAZ-MELLO S.
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Planetary system LHS 1140 revisited with ESPRESSO and TESS
2020 LILLO-BOX J., FIGUEIRA P., LELEU A., ACUÑA L., FARIA J. et al.
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Astron. J., 157, 32
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A search for technosignatures from TRAPPIST-1, LHS 1140, and 10 planetary systems in the Kepler field with the Green Bank Telescope at 1.15-1.73 GHz
2019 PINCHUK P., MARGOT J.-L., GREENBERG A., AYALDE Th., BLOXHAM Ch. et al.
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Detectability of atmospheric features of Earth-like planets in the habitable zone around M dwarfs
2019 WUNDERLICH F., GODOLT M., GRENFELL J., STÄDT S., SMITH A. et al.
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2019 O'MALLEY-JAMES J. & KALTENEGGER L.
MNRAS, accepted
arxiv  

The high-energy radiation environment of the habitable-zone super-Earth LHS 1140b
2019 SPINELLI R., BORSA F., GHIRLANDA G., GHISELLINI G.,CAMPANA S. et al.
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