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An ablating 2.6 M ⊕ planet in an eccentric binary from the Dispersed Matter Planet Project
Nature Astronomy ( IF 10.500 ) Pub Date : 2019-12-23 , DOI: 10.1038/s41550-019-0972-z
John R. Barnes; Carole A. Haswell; Daniel Staab; Guillem Anglada-Escudé; Luca Fossati; James P. J. Doherty; Joseph Cooper; James S. Jenkins; Matías R. Díaz; Maritza G. Soto; Pablo A. Peña Rojas

Earth-mass exoplanets are difficult to detect. The Dispersed Matter Planet Project (DMPP) identifies stars that are likely to host the most detectable low-mass exoplanets. The star DMPP-3 (HD 42936) shows signs of circumstellar absorption, indicative of mass loss from ablating planets. Here, we report the radial velocity discovery of a highly eccentric 507 d binary companion and a hot super-Earth-mass planet in a 6.67 d orbit around the primary star. DMPP-3A is a solar-type star while DMPP-3B is just massive enough to fuse hydrogen. The binary, with semi-major axis 1.22 ± 0.02 au, is considerably tighter than others known to host planets orbiting only one of the component stars. The configuration of the DMPP-3 planetary system is rare and indicates dynamical interactions, though the evolutionary history is not entirely clear. DMPP-3A b is possibly the residual core of a giant planet precursor, consistent with the inferred circumstellar gas shroud.
更新日期:2019-12-23

 

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