THE FIRST NEPTUNE ANALOG OR SUPER-EARTH WITH A NEPTUNE-LIKE ORBIT: MOA-2013-BLG-605LB

THE FIRST NEPTUNE ANALOG OR SUPER-EARTH WITH A NEPTUNE-LIKE ORBIT: MOA-2013-BLG-605LB
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DOI：
10.3847/0004-637x/825/2/112
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发表时间：
2015-12
期刊：
The Astrophysical Journal
影响因子：
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通讯作者：
T. Sumi;A. Udalski;D. Bennett;A. Gould;R. Poleski;I. Bond;J. Skowron;N. Rattenbury;R. Pogge;T. Bensby;J. Beaulieu;J. Marquette;V. Batista;S. Brillant;F. Abe;Y. Asakura;A. Bhattacharya;M. Donachie;M. Freeman;A. Fukui;Y. Hirao;Y. Itow;N. Koshimoto;M. Li;C. Ling;K. Masuda;Y. Matsubara;Y. Muraki;M. Nagakane;K. Ohnishi;H. Oyokawa;T. Saito;A. Sharan;D. Sullivan;D. Suzuki;P. Tristram;A. Yonehara;M. Szymański;K. Ulaczyk;S. Kozłowski;Ł. Wyrzykowski;M. Kubiak;P. Pietrukowicz;G. Pietrzyński;I. Soszyński;C. Han;Y. Jung;I. Shin;C.‐U. Lee
T. Sumi;A. Udalski;D. Bennett;A. Gould;R. Poleski;I. Bond;J. Skowron;N. Rattenbury;R. Pogge;T. Bensby;J. Beaulieu;J. Marquette;V. Batista;S. Brillant;F. Abe;Y. Asakura;A. Bhattacharya;M. Donachie;M. Freeman;A. Fukui;Y. Hirao;Y. Itow;N. Koshimoto;M. Li;C. Ling;K. Masuda;Y. Matsubara;Y. Muraki;M. Nagakane;K. Ohnishi;H. Oyokawa;T. Saito;A. Sharan;D. Sullivan;D. Suzuki;P. Tristram;A. Yonehara;M. Szymański;K. Ulaczyk;S. Kozłowski;Ł. Wyrzykowski;M. Kubiak;P. Pietrukowicz;G. Pietrzyński;I. Soszyński;C. Han;Y. Jung;I. Shin;C.‐U. Lee
中科院分区：
其他
文献类型：
--
作者：
T. Sumi;A. Udalski;D. Bennett;A. Gould;R. Poleski;I. Bond;J. Skowron;N. Rattenbury;R. Pogge;T. Bensby;J. Beaulieu;J. Marquette;V. Batista;S. Brillant;F. Abe;Y. Asakura;A. Bhattacharya;M. Donachie;M. Freeman;A. Fukui;Y. Hirao;Y. Itow;N. Koshimoto;M. Li;C. Ling;K. Masuda;Y. Matsubara;Y. Muraki;M. Nagakane;K. Ohnishi;H. Oyokawa;T. Saito;A. Sharan;D. Sullivan;D. Suzuki;P. Tristram;A. Yonehara;M. Szymański;K. Ulaczyk;S. Kozłowski;Ł. Wyrzykowski;M. Kubiak;P. Pietrukowicz;G. Pietrzyński;I. Soszyński;C. Han;Y. Jung;I. Shin;C.‐U. Lee

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We present the discovery of the first Neptune analog exoplanet or super-Earth with a Neptune-like orbit, MOA-2013-BLG-605Lb. This planet has a mass similar to that of Neptune or a super-Earth and it orbits at 9 ∼ 14 times the expected position of the snow line, asnow, which is similar to Neptune's separation of 11 asnow from the Sun. The planet/host-star mass ratio is q = (3.6 ± 0.7) × 10−4 and the projected separation normalized by the Einstein radius is s = 2.39 ± 0.05. There are three degenerate physical solutions and two of these are due to a new type of degeneracy in the microlensing parallax parameters, which we designate “the wide degeneracy.” The three models have (i) a Neptune-mass planet with a mass of orbiting a low-mass M-dwarf with a mass of , (ii) a mini-Neptune with orbiting a brown dwarf host with , and (iii) a super-Earth with orbiting a low-mass brown dwarf host with , which is slightly favored. The 3D planet–host separations are au, au, and au, which are , , or times larger than asnow for these models, respectively. Keck adaptive optics observations confirm that the lens is faint. This discovery suggests that low-mass planets with Neptune-like orbits are common. Therefore processes similar to the one that formed Neptune in our own solar system or cold super-Earths may be common in other solar systems.