Abstract
It is commonly accepted that exoplanets with orbital periods shorter than one day, also known as ultra-short-period (USP) planets, formed further out within their natal protoplanetary disks before migrating to their current-day orbits via dynamical interactions. One of the most accepted theories suggests a violent scenario involving high-eccentricity migration followed by tidal circularization. Here we present the discovery of a four-planet system orbiting the bright (V = 10.5) K6 dwarf star TOI-500. The innermost planet is a transiting, Earth-sized USP planet with an orbital period of ~13 hours, a mass of 1.42 ± 0.18 M⊕, a radius of 1.166−0.058+0.061R⊕ and a mean density of 4.89−0.88+1.03gcm−3. Via Doppler spectroscopy, we discovered that the system hosts 3 outer planets on nearly circular orbits with periods of 6.6, 26.2 and 61.3 days and minimum masses of 5.03 ± 0.41 M⊕, 33.12 ± 0.88 M⊕ and 15.05−1.11+1.12M⊕, respectively. The presence of both a USP planet and a low-mass object on a 6.6-day orbit indicates that the architecture of this system can be explained via a scenario in which the planets started on low-eccentricity orbits then moved inwards through a quasi-static secular migration. Our numerical simulations show that this migration channel can bring TOI-500 b to its current location in 2 Gyr, starting from an initial orbit of 0.02 au. TOI-500 is the first four-planet system known to host a USP Earth analogue whose current architecture can be explained via a non-violent migration scenario.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 736-750 |
| Number of pages | 15 |
| Journal | Nature Astronomy |
| Volume | 6 |
| Issue number | 6 |
| DOIs | |
| State | Published - Jun 2022 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
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In: Nature Astronomy, Vol. 6, No. 6, 06.2022, p. 736-750.
Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - A low-eccentricity migration pathway for a 13-h-period Earth analogue in a four-planet system
AU - Serrano, Luisa Maria
AU - Gandolfi, Davide
AU - Mustill, Alexander J.
AU - Barragán, Oscar
AU - Korth, Judith
AU - Dai, Fei
AU - Redfield, Seth
AU - Fridlund, Malcolm
AU - Lam, Kristine W.F.
AU - Díaz, Matías R.
AU - Grziwa, Sascha
AU - Collins, Karen A.
AU - Livingston, John H.
AU - Cochran, William D.
AU - Hellier, Coel
AU - Bellomo, Salvatore E.
AU - Trifonov, Trifon
AU - Rodler, Florian
AU - Alarcon, Javier
AU - Jenkins, Jon M.
AU - Latham, David W.
AU - Ricker, George
AU - Seager, Sara
AU - Vanderspeck, Roland
AU - Winn, Joshua N.
AU - Albrecht, Simon
AU - Collins, Kevin I.
AU - Csizmadia, Szilárd
AU - Daylan, Tansu
AU - Deeg, Hans J.
AU - Esposito, Massimiliano
AU - Fausnaugh, Michael
AU - Georgieva, Iskra
AU - Goffo, Elisa
AU - Guenther, Eike
AU - Hatzes, Artie P.
AU - Howell, Steve B.
AU - Jensen, Eric L.N.
AU - Luque, Rafael
AU - Mann, Andrew W.
AU - Murgas, Felipe
AU - Osborne, Hannah L.M.
AU - Palle, Enric
AU - Persson, Carina M.
AU - Rowden, Pam
AU - Rudat, Alexander
AU - Smith, Alexis M.S.
AU - Twicken, Joseph D.
AU - Van Eylen, Vincent
AU - Ziegler, Carl
N1 - Funding Information: This work was supported by the KESPRINT ( www.kesprint.science ) collaboration, an international consortium devoted to the characterization and research of exoplanets discovered with space-based missions. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. We acknowledge the use of TESS Alert data, which is currently in a beta test phase, from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing Program through the NASA Advanced Supercomputing Division at Ames Research Center for the production of the SPOC data products. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work makes use of observations made with the ESO 3.6 m telescope at the European Southern Observatory (ESO), La Silla, under ESO programmes 1102.C-0923, 0102.C-0338, 0103.C-0442, 0103.C-0548, 60.A-9700 and 60.A-9709. We are very grateful to the ESO staff members for their precious support during the observations. We warmly thank X. Dumusque and F. Bouchy for coordinating the shared observations with HARPS and J. Alvarado Montes, X. Delfosse, G. Gaisné, M. Hobson and D. Barrado Navascués, who helped collecting the HARPS spectra. This work has made use of data from the European Space Agency mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium ( https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the Data Processing and Analysis Consortium has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work makes use of observations from the LCOGT network. LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program, which is funded by the National Science Foundation. Some of the observations in the paper made use of the high-resolution imaging instrument Zorro. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by S. B. Howell, N. Scott, E. P. Horch and E. Quigley. Data was reduced using a software pipeline originally written by E. Horch and M. Everett. Zorro was mounted on the Gemini South telescope and the Near Infrared Imager (NIRI) was mounted on the Gemini North telescope, of the international Gemini Observatory, a programme of the National Science Foundation’s OIR Lab, which is managed by the Association of Universities for Research in Astronomy under a cooperative agreement with the National Science Foundation on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil) and Korea Astronomy and Space Science Institute (Republic of Korea). Data collected under programme GN-2019A-LP-101. This work was based in part on observations obtained at the SOAR telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina at Chapel Hill and Michigan State University. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. L.M.S. and D.G. gratefully acknowledge financial support from the CRT foundation under Grant No. 2018.2323 “Gaseous or rocky? Unveiling the nature of small worlds.” E.Gu. acknowledges the generous support by the Thüringer Ministerium für Wirtschaft, Wissenschaft und Digitale Gesellschaft. I.G., C.M.P., M.Fr. and A.J.M. gratefully acknowledge the support of the Swedish National Space Agency (DNR 174/18, 65/19, 120/19C). J.K. gratefully acknowledges the support of the Swedish National Space Agency (DNR 2020-00104). S.C., M.E., K.W.F.L., S.G. and A.P.H. acknowledge support by DFG grants RA714/14-1 within the DFG Schwerpunkt SPP 1992, “Exploring the Diversity of Extrasolar Planets”. M.R.D. acknowledges the support by Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)-PFCHA/Doctorado Nacional-21140646, Chile. T.D. acknowledges support from MIT’s Kavli Institute as Kavli postdoctoral fellow. T.T. acknowledges support by the DFG Research Unit FOR 2544 “Blue Planets around Red Stars" project No. KU 3625/2-1. T.T. further acknowledges support by the BNSF programme “VIHREN-2021" project No. КП-06-ДВ/5. Funding Information: This work was supported by the KESPRINT (www.kesprint.science) collaboration, an international consortium devoted to the characterization and research of exoplanets discovered with space-based missions. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. We acknowledge the use of TESS Alert data, which is currently in a beta test phase, from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing Program through the NASA Advanced Supercomputing Division at Ames Research Center for the production of the SPOC data products. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work makes use of observations made with the ESO 3.6 m telescope at the European Southern Observatory (ESO), La Silla, under ESO programmes 1102.C-0923, 0102.C-0338, 0103.C-0442, 0103.C-0548, 60.A-9700 and 60.A-9709. We are very grateful to the ESO staff members for their precious support during the observations. We warmly thank X. Dumusque and F. Bouchy for coordinating the shared observations with HARPS and J. Alvarado Montes, X. Delfosse, G. Gaisné, M. Hobson and D. Barrado Navascués, who helped collecting the HARPS spectra. This work has made use of data from the European Space Agency mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the Data Processing and Analysis Consortium has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work makes use of observations from the LCOGT network. LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program, which is funded by the National Science Foundation. Some of the observations in the paper made use of the high-resolution imaging instrument Zorro. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by S. B. Howell, N. Scott, E. P. Horch and E. Quigley. Data was reduced using a software pipeline originally written by E. Horch and M. Everett. Zorro was mounted on the Gemini South telescope and the Near Infrared Imager (NIRI) was mounted on the Gemini North telescope, of the international Gemini Observatory, a programme of the National Science Foundation’s OIR Lab, which is managed by the Association of Universities for Research in Astronomy under a cooperative agreement with the National Science Foundation on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil) and Korea Astronomy and Space Science Institute (Republic of Korea). Data collected under programme GN-2019A-LP-101. This work was based in part on observations obtained at the SOAR telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina at Chapel Hill and Michigan State University. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. L.M.S. and D.G. gratefully acknowledge financial support from the CRT foundation under Grant No. 2018.2323 “Gaseous or rocky? Unveiling the nature of small worlds.” E.Gu. acknowledges the generous support by the Thüringer Ministerium für Wirtschaft, Wissenschaft und Digitale Gesellschaft. I.G., C.M.P., M.Fr. and A.J.M. gratefully acknowledge the support of the Swedish National Space Agency (DNR 174/18, 65/19, 120/19C). J.K. gratefully acknowledges the support of the Swedish National Space Agency (DNR 2020-00104). S.C., M.E., K.W.F.L., S.G. and A.P.H. acknowledge support by DFG grants RA714/14-1 within the DFG Schwerpunkt SPP 1992, “Exploring the Diversity of Extrasolar Planets”. M.R.D. acknowledges the support by Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)-PFCHA/Doctorado Nacional-21140646, Chile. T.D. acknowledges support from MIT’s Kavli Institute as Kavli postdoctoral fellow. T.T. acknowledges support by the DFG Research Unit FOR 2544 “Blue Planets around Red Stars" project No. KU 3625/2-1. T.T. further acknowledges support by the BNSF programme “VIHREN-2021" project No. КП-06-ДВ/5. Publisher Copyright: © 2022, The Author(s), under exclusive licence to Springer Nature Limited.
PY - 2022/6
Y1 - 2022/6
N2 - It is commonly accepted that exoplanets with orbital periods shorter than one day, also known as ultra-short-period (USP) planets, formed further out within their natal protoplanetary disks before migrating to their current-day orbits via dynamical interactions. One of the most accepted theories suggests a violent scenario involving high-eccentricity migration followed by tidal circularization. Here we present the discovery of a four-planet system orbiting the bright (V = 10.5) K6 dwarf star TOI-500. The innermost planet is a transiting, Earth-sized USP planet with an orbital period of ~13 hours, a mass of 1.42 ± 0.18 M⊕, a radius of 1.166−0.058+0.061R⊕ and a mean density of 4.89−0.88+1.03gcm−3. Via Doppler spectroscopy, we discovered that the system hosts 3 outer planets on nearly circular orbits with periods of 6.6, 26.2 and 61.3 days and minimum masses of 5.03 ± 0.41 M⊕, 33.12 ± 0.88 M⊕ and 15.05−1.11+1.12M⊕, respectively. The presence of both a USP planet and a low-mass object on a 6.6-day orbit indicates that the architecture of this system can be explained via a scenario in which the planets started on low-eccentricity orbits then moved inwards through a quasi-static secular migration. Our numerical simulations show that this migration channel can bring TOI-500 b to its current location in 2 Gyr, starting from an initial orbit of 0.02 au. TOI-500 is the first four-planet system known to host a USP Earth analogue whose current architecture can be explained via a non-violent migration scenario.
AB - It is commonly accepted that exoplanets with orbital periods shorter than one day, also known as ultra-short-period (USP) planets, formed further out within their natal protoplanetary disks before migrating to their current-day orbits via dynamical interactions. One of the most accepted theories suggests a violent scenario involving high-eccentricity migration followed by tidal circularization. Here we present the discovery of a four-planet system orbiting the bright (V = 10.5) K6 dwarf star TOI-500. The innermost planet is a transiting, Earth-sized USP planet with an orbital period of ~13 hours, a mass of 1.42 ± 0.18 M⊕, a radius of 1.166−0.058+0.061R⊕ and a mean density of 4.89−0.88+1.03gcm−3. Via Doppler spectroscopy, we discovered that the system hosts 3 outer planets on nearly circular orbits with periods of 6.6, 26.2 and 61.3 days and minimum masses of 5.03 ± 0.41 M⊕, 33.12 ± 0.88 M⊕ and 15.05−1.11+1.12M⊕, respectively. The presence of both a USP planet and a low-mass object on a 6.6-day orbit indicates that the architecture of this system can be explained via a scenario in which the planets started on low-eccentricity orbits then moved inwards through a quasi-static secular migration. Our numerical simulations show that this migration channel can bring TOI-500 b to its current location in 2 Gyr, starting from an initial orbit of 0.02 au. TOI-500 is the first four-planet system known to host a USP Earth analogue whose current architecture can be explained via a non-violent migration scenario.
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U2 - 10.1038/s41550-022-01641-y
DO - 10.1038/s41550-022-01641-y
M3 - Article
AN - SCOPUS:85129057819
SN - 2397-3366
VL - 6
SP - 736
EP - 750
JO - Nature Astronomy
JF - Nature Astronomy
IS - 6
ER -