| Autor: |
Jeffrey C. Smith, Philipp Eigmüller, Edward H. Morgan, Sebastiano Padovan, Massimiliano Esposito, Felipe Murgas, Robert L. Morris, Jessie L. Christiansen, Jan Subjak, Alexander Chaushev, Rafael Luque, William D. Cochran, Iskra Georgieva, Nuno C. Santos, Enric Palle, Damien Ségransan, Malcolm Fridlund, George R. Ricker, René Doyon, Priyanka Chaturvedi, Samuel N. Quinn, Vincent Van Eylen, Judith Korth, Marshall C. Johnson, Guillaume Gaisné, Hannah L. M. Osborne, Michel Mayor, Eike W. Guenther, Pablo Lewin, Joshua E. Schlieder, Norio Narita, Oscar Barragán, Etienne Artigau, Thierry Forveille, Roland Vanderspek, Joshua N. Winn, Simon Albrecht, Artie P. Hatzes, Juan Cabrera, E. Goffo, Jack J. Lissauer, Steve B. Howell, P. Figueira, José R. De Meideiros, Joseph D. Twicken, David Charbonneau, Szilard Csizmadia, Savita Mathur, Alexis M. S. Smith, Seth Redfield, Sascha Grziwa, Luisa M. Serrano, Xavier Delfosse, Rodrigo F. Díaz, Fei Dai, Rafael A. García, Stéphane Udry, Jon M. Jenkins, Petr Kabath, Emil Knudstrup, Kristine W F Lam, Francesco Pepe, François Bouchy, Coel Hellier, Carina M. Persson, Davide Gandolfi, Jose M Almenara, Sara Seager, Karen A. Collins, Nicola Astudillo-Defru, Heike Rauer, David W. Latham, Teruyuki Hirano, Michael Vezie, John H. Livingston, Claudio Melo, Christophe Lovis, X. Bonfils |
| Jazyk: |
angličtina |
| Rok vydání: |
2021 |
| Předmět: |
|
| Zdroj: |
Science, 374(6572), 1271-1275 |
| ISSN: |
0036-8075 |
| Popis: |
Ultra-short-period (USP) exoplanets have orbital periods shorter than one day. Precise masses and radii of USPs could provide constraints on their unknown formation and evolution processes. We report the detection and characterization of the USP planet GJ 367b using high precision photometry and radial velocity observations. GJ 367b orbits a bright (V-band magnitude = 10.2), nearby, red (M-type) dwarf star every 7.7 hours. GJ 367b has a radius of $0.718 \pm 0.054$ Earth-radii, a mass of $0.546 \pm 0.078$ Earth-masses, making it a sub-Earth. The corresponding bulk density is $8.106 \pm 2.165$ g cm$^-3$, close to that of iron. An interior structure model predicts the planet has an iron core radius fraction of $86 \pm 5\%$, similar to Mercury's interior.
Comment: Note: "This is the author's version of the work. It is posted here by permission of the AAAS for personal use, not for redistribution. The definitive version was published in Science , (2021-12-03), doi: 10.1126/science.aay3253" |
| Databáze: |
OpenAIRE |
| Externí odkaz: |
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