Forming Gas Giants around a Range of Protostellar M-dwarfs by Gas Disk Gravitational Instability
Recent discoveries of gas giant exoplanets around M-dwarfs from transiting and radial velocity surveys are difficult to explain with core-accretion models. We present here a homogeneous suite of 162 models of gravitationally unstable gaseous disks. These models represent an existence proof for gas g...
| Main Authors: | , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/acf373 |
| _version_ | 1797670622269014016 |
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| author | Alan P. Boss Shubham Kanodia |
| author_facet | Alan P. Boss Shubham Kanodia |
| author_sort | Alan P. Boss |
| collection | DOAJ |
| description | Recent discoveries of gas giant exoplanets around M-dwarfs from transiting and radial velocity surveys are difficult to explain with core-accretion models. We present here a homogeneous suite of 162 models of gravitationally unstable gaseous disks. These models represent an existence proof for gas giants more massive than 0.1 Jupiter masses to form by the gas disk gravitational instability (GDGI) mechanism around M-dwarfs for comparison with observed exoplanet demographics and protoplanetary disk mass estimates for M-dwarf stars. We use the Enzo 2.6 adaptive mesh refinement (AMR) 3D hydrodynamics code to follow the formation and initial orbital evolution of gas giant protoplanets in gravitationally unstable gaseous disks in orbit around M-dwarfs with stellar masses ranging from 0.1 M _⊙ to 0.5 M _⊙ . The gas disk masses are varied over a range from disks that are too low in mass to form gas giants rapidly to those where numerous gas giants are formed, therefore revealing the critical disk mass necessary for gas giants to form by the GDGI mechanism around M-dwarfs. The disk masses vary from 0.01 M _⊙ to 0.05 M _⊙ while the disk to star mass ratios explored the range from 0.04 to 0.3. The models have varied initial outer disk temperatures (10–60 K) and varied levels of AMR grid spatial resolution, producing a sample of expected gas giant protoplanets for each star mass. Broadly speaking, disk masses of at least 0.02 M _⊙ are needed for the GDGI mechanism to form gas giant protoplanets around M-dwarfs. |
| first_indexed | 2024-03-11T21:03:13Z |
| format | Article |
| id | doaj.art-0f5be9fd017247ec9b782799a6bd46a9 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-11T21:03:13Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-0f5be9fd017247ec9b782799a6bd46a92023-09-29T17:33:41ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-019561410.3847/1538-4357/acf373Forming Gas Giants around a Range of Protostellar M-dwarfs by Gas Disk Gravitational InstabilityAlan P. Boss0https://orcid.org/0000-0001-7119-1105Shubham Kanodia1https://orcid.org/0000-0001-8401-4300Earth & Planets Laboratory, Carnegie Institution for Science , 5241 Broad Branch Road, NW, Washington, DC 20015-1305, USA ; aboss@carnegiescience.eduEarth & Planets Laboratory, Carnegie Institution for Science , 5241 Broad Branch Road, NW, Washington, DC 20015-1305, USA ; aboss@carnegiescience.eduRecent discoveries of gas giant exoplanets around M-dwarfs from transiting and radial velocity surveys are difficult to explain with core-accretion models. We present here a homogeneous suite of 162 models of gravitationally unstable gaseous disks. These models represent an existence proof for gas giants more massive than 0.1 Jupiter masses to form by the gas disk gravitational instability (GDGI) mechanism around M-dwarfs for comparison with observed exoplanet demographics and protoplanetary disk mass estimates for M-dwarf stars. We use the Enzo 2.6 adaptive mesh refinement (AMR) 3D hydrodynamics code to follow the formation and initial orbital evolution of gas giant protoplanets in gravitationally unstable gaseous disks in orbit around M-dwarfs with stellar masses ranging from 0.1 M _⊙ to 0.5 M _⊙ . The gas disk masses are varied over a range from disks that are too low in mass to form gas giants rapidly to those where numerous gas giants are formed, therefore revealing the critical disk mass necessary for gas giants to form by the GDGI mechanism around M-dwarfs. The disk masses vary from 0.01 M _⊙ to 0.05 M _⊙ while the disk to star mass ratios explored the range from 0.04 to 0.3. The models have varied initial outer disk temperatures (10–60 K) and varied levels of AMR grid spatial resolution, producing a sample of expected gas giant protoplanets for each star mass. Broadly speaking, disk masses of at least 0.02 M _⊙ are needed for the GDGI mechanism to form gas giant protoplanets around M-dwarfs.https://doi.org/10.3847/1538-4357/acf373Extrasolar gaseous giant planetsProtoplanetary disksGravitational instability |
| spellingShingle | Alan P. Boss Shubham Kanodia Forming Gas Giants around a Range of Protostellar M-dwarfs by Gas Disk Gravitational Instability The Astrophysical Journal Extrasolar gaseous giant planets Protoplanetary disks Gravitational instability |
| title | Forming Gas Giants around a Range of Protostellar M-dwarfs by Gas Disk Gravitational Instability |
| title_full | Forming Gas Giants around a Range of Protostellar M-dwarfs by Gas Disk Gravitational Instability |
| title_fullStr | Forming Gas Giants around a Range of Protostellar M-dwarfs by Gas Disk Gravitational Instability |
| title_full_unstemmed | Forming Gas Giants around a Range of Protostellar M-dwarfs by Gas Disk Gravitational Instability |
| title_short | Forming Gas Giants around a Range of Protostellar M-dwarfs by Gas Disk Gravitational Instability |
| title_sort | forming gas giants around a range of protostellar m dwarfs by gas disk gravitational instability |
| topic | Extrasolar gaseous giant planets Protoplanetary disks Gravitational instability |
| url | https://doi.org/10.3847/1538-4357/acf373 |
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