Exoplanets around Low-mass Stars Unveiled by K2

被引：72

作者：

Hirano, Teruyuki ^{[1
]}

Dai, Fei ^{[2
,3
,4
]}

Gandolfi, Davide ^{[5
]}

Fukui, Akihiko ^{[6
]}

Livingston, John H. ^{[7
]}

Miyakawa, Kohei ^{[1
]}

Endl, Michael ^{[8
,9
]}

Cochran, William D. ^{[8
,9
]}

Alonso-Floriano, Francisco J. ^{[10
,11
]}

Kuzuhara, Masayuki ^{[12
,13
]}

Montes, David ^{[11
]}

Ryu, Tsuguru ^{[13
,14
]}

Albrecht, Simon ^{[15
]}

Barragan, Oscar ^{[5
]}

Cabrera, Juan ^{[16
]}

Csizmadia, Szilard ^{[16
]}

Deeg, Hans ^{[17
,18
]}

Eigmueller, Philipp ^{[16
]}

Erikson, Anders ^{[16
]}

Fridlund, Malcolm ^{[10
,19
]}

Grziwa, Sascha ^{[20
]}

Guenther, Eike W. ^{[21
]}

Hatzes, Artie P. ^{[21
]}

Korth, Judith ^{[20
]}

Kudo, Tomoyuki ^{[22
]}

Kusakabe, Nobuhiko ^{[12
,13
]}

Narita, Norio ^{[7
,12
,13
]}

Nespral, David ^{[17
,18
]}

Nowak, Grzegorz ^{[17
,18
]}

Paetzold, Martin ^{[20
]}

Palle, Enric ^{[17
,18
]}

Persson, Carina M. ^{[19
]}

Prieto-Arranz, Jorge ^{[17
,18
]}

Rauer, Heike ^{[16
,23
]}

Ribas, Ignasi ^{[24
]}

Sato, Bun'ei ^{[1
]}

Smith, Alexis M. S. ^{[16
]}

Tamura, Motohide ^{[7
,12
,13
]}

Tanaka, Yusuke ^{[7
]}

Van Eylen, Vincent ^{[10
]}

Winn, Joshua N. ^{[4
]}

机构：

[1] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan

[2] MIT, Dept Phys, Cambridge, MA 02139 USA

[3] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA

[4] Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08544 USA

[5] Univ Turin, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy

[6] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan

[7] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Hongo 7-3-1, Tokyo 1130033, Japan

[8] Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1400, Austin, TX 78712 USA

[9] Univ Texas Austin, McDonald Observ, 2515 Speedway,Stop C1400, Austin, TX 78712 USA

[10] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands

[11] Univ Complutense Madrid, Fac Ciencias Fis, Dept Astrofis & Ciencias Atmosfera, E-28040 Madrid, Spain

[12] NINS, Astrobiol Ctr, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[13] NINS, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[14] SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[15] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark

[16] German Aerosp Ctr, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany

[17] Inst Astrofis Canarias, C Via Lactea S-N, E-38205 San Cristobal la Laguna, Spain

[18] Univ La Laguna, Dept Astrofis, E-38206 San Cristobal la Laguna, Spain

[19] Chalmers Univ Technol, Onsala Space Observ, Dept Space Earth & Environm, SE-43992 Onsala, Sweden

[20] Univ Cologne, Rhein Inst Umweltforsch, Aachener Str 209, D-50931 Cologne, Germany

[21] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany

[22] Natl Astron Observ Japan, Subaru Telescope, 650 North Aohoku Pl, Hilo, HI 96720 USA

[23] TU Berlin, Ctr Astron & Astrophys, Hardenbergstr 36, D-10623 Berlin, Germany

[24] CSIC IEEC, Inst Ciencies Espai, Campus UAB, E-08193 Bellaterra, Spain

来源：

ASTRONOMICAL JOURNAL | 2018年 / 155卷 / 03期

关键词：

methods: observational; planets and satellites: detection; techniques: high angular resolution; techniques: photometric; techniques: radial velocities; techniques: spectroscopic; SUPER-EARTH; PLANETARY; STELLAR; SPECTROGRAPH; PARAMETERS; SYSTEMS; RADIUS; VALIDATION; CANDIDATES; TARGETS;

D O I：

10.3847/1538-3881/aaa9c1

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the detection and follow-up observations of planetary candidates around low-mass stars observed by the K2 mission. Based on light-curve analysis, adaptive-optics imaging, and optical spectroscopy at low and high resolution (including radial velocity measurements), we validate 16 planets around 12 low-mass stars observed during K2 campaigns 5-10. Among the 16 planets, 12 are newly validated, with orbital periods ranging from 0.96 to 33 days. For one of the planets (K2-151b), we present ground-based transit photometry, allowing us to refine the ephemerides. Combining our K2 M-dwarf planets together with the validated or confirmed planets found previously, we investigate the dependence of planet radius R-p on stellar insolation and metallicity [Fe/H]. We confirm that for periods P less than or similar to 2 days, planets with a radius R-p greater than or similar to 2 R-circle plus are less common than planets with a radius between 1-2 R-circle plus. We also see a hint of the "radius valley" between 1.5 and 2 R-circle plus, which has been seen for close-in planets around FGK stars. These features in the radius/period distribution could be attributed to photoevaporation of planetary envelopes by high-energy photons from the host star, as they have for FGK stars. For the M dwarfs, though, the features are not as well defined, and we cannot rule out other explanations such as atmospheric loss from internal planetary heat sources or truncation of the protoplanetary disk. There also appears to be a relation between planet size and metallicity: the few planets larger than about 3 R-circle plus are found around the most metal-rich M dwarfs.

引用

页数：23

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