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Discovery | |
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Discovered by | Mikko Tuomi et al. |
Discovery site | La Silla Observatory, Chile |
Discovery date | October 28, 2012 |
radial velocity, using HARPS | |
Orbital characteristics | |
0.1886 [0.1782, 0.1969] AU | |
Eccentricity | 0.06 [0, 0.18] [1] |
34.62 [34.42, 34.83] [1] d | |
Semi-amplitude | 0.84 [0.53, 1.16] [1] |
Star | HD 40307 |
HD 40307 e is an extrasolar planet candidate suspected to be orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus [1] [2] [3] by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of Göttingen, Germany. [4]
The existence of the planet was disputed in 2015, as more Doppler spectroscopy data has become available. [5]
Its minimum mass is 3.5 that of Earth - the smallest - and dynamical models suggest it cannot be much more (and so is measured close to edge-on). [1] It further gets roughly the same insolation from its star as Mercury gets from the Sun. [6] Planets like this in that system have been presumed "super-Earth". [7]
However planets b, c, and d are presumed to have migrated in from outer orbits; and planet b is predicted a sub-Neptune. [8] It is likely that this planet formed even further out. Whether it is a sub-Neptune, a super-Venus or even a super-Mercury is unknown.
![]() | |
Discovery | |
---|---|
Discovered by | Mikko Tuomi et al. |
Discovery site | La Silla Observatory, Chile |
Discovery date | October 28, 2012 |
radial velocity, using HARPS | |
Orbital characteristics | |
0.1886 [0.1782, 0.1969] AU | |
Eccentricity | 0.06 [0, 0.18] [1] |
34.62 [34.42, 34.83] [1] d | |
Semi-amplitude | 0.84 [0.53, 1.16] [1] |
Star | HD 40307 |
HD 40307 e is an extrasolar planet candidate suspected to be orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus [1] [2] [3] by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of Göttingen, Germany. [4]
The existence of the planet was disputed in 2015, as more Doppler spectroscopy data has become available. [5]
Its minimum mass is 3.5 that of Earth - the smallest - and dynamical models suggest it cannot be much more (and so is measured close to edge-on). [1] It further gets roughly the same insolation from its star as Mercury gets from the Sun. [6] Planets like this in that system have been presumed "super-Earth". [7]
However planets b, c, and d are presumed to have migrated in from outer orbits; and planet b is predicted a sub-Neptune. [8] It is likely that this planet formed even further out. Whether it is a sub-Neptune, a super-Venus or even a super-Mercury is unknown.