History and Habitability of the LP 890-9 Planetary System

Rory Barnes; Laura N.R. do Amaral; Jessica Birky; Ludmila Carone; Peter Driscoll; Joseph R. Livesey; David Graham; Juliette Becker; Kaiming Cui; Martin Schlecker; Rodolfo Garcia; Megan Gialluca; Arthur Adams; MD Redyan Ahmed; Paul Bonney; Wynter Broussard; Chetan Chawla; Mario Damasso; William C. Danchi; Russell Deitrick; Elsa Ducrot; Emeline F. Fromont; Brandt A.L. Gaches; Sakshi Gupta; Michelle L. Hill; James A.G. Jackman; Estelle M. Janin; Mikołaj Karawacki; Matheus Daniel Koren; Roberto La Greca; Michaela Leung; Arturo Miranda-Rosete; Michael Kent A. Olohoy; Cecelia Ngo; Daria Paul; Chandan Kumar Sahu; Debajyoti Basu Sarkar; Mohammad Afzal Shadab; Edward W. Schwieterman; Melissa Sedler; Katie Texeira; Allona Vazan; Karen N. Delgado Vega; Rohit Vijayakumar; Jonathan T. Wojack

doi:10.3847/PSJ/ad94dc

History and Habitability of the LP 890-9 Planetary System

Rory Barnes, Laura N.R. do Amaral, Jessica Birky, Ludmila Carone, Peter Driscoll, Joseph R. Livesey, David Graham, Juliette Becker, Kaiming Cui, Martin Schlecker, Rodolfo Garcia, Megan Gialluca, Arthur Adams, MD Redyan Ahmed, Paul Bonney, Wynter Broussard, Chetan Chawla, Mario Damasso, William C. Danchi, Russell DeitrickElsa Ducrot, Emeline F. Fromont, Brandt A.L. Gaches, Sakshi Gupta, Michelle L. Hill, James A.G. Jackman, Estelle M. Janin, Mikołaj Karawacki, Matheus Daniel Koren, Roberto La Greca, Michaela Leung, Arturo Miranda-Rosete, Michael Kent A. Olohoy, Cecelia Ngo, Daria Paul, Chandan Kumar Sahu, Debajyoti Basu Sarkar, Mohammad Afzal Shadab, Edward W. Schwieterman, Melissa Sedler, Katie Texeira, Allona Vazan, Karen N. Delgado Vega, Rohit Vijayakumar, Jonathan T. Wojack

Physics

Research output: Contribution to journal › Article › peer-review

Abstract

We present numerous aspects of the evolution of the LP 890-9 (SPECULOOS-2/TOI-4306) planetary system, focusing on the likelihood that planet c can support life. We find that the host star reaches the main sequence in 1 Gyr and that planet c lies close to the inner boundary of the habitable zone. We find the magma ocean stage can last up to 50 Myr, remove eight Earth oceans of water, and leave up to 2000 bars of oxygen in the atmosphere. However, if the planet forms with a hydrogen envelope as small as 0.1 Earth masses, no water will be lost during the star's pre-main-sequence phase from thermal escape processes. We find that the planets are unlikely to be in a 3:1 mean motion resonance and that both planets tidally circularize within 0.5 Gyr when tidal dissipation is held constant. However, if tidal dissipation is a function of mantle temperature and rheology, then we find that planet c's orbit may require more than 7 Gyr to circularize, during which time tidal heating may reach hundreds of terawatts. We thus conclude that the habitability of planet c depends most strongly on the initial volatile content and internal properties, but no data yet preclude the viability of an active biosphere on the planet.

Original language	English
Article number	25
Journal	Planetary Science Journal
Volume	6
Issue number	1
DOIs	https://doi.org/10.3847/PSJ/ad94dc
State	Published - 1 Jan 2025

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Publisher Copyright:
© 2025. The Author(s). Published by the American Astronomical Society.

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Barnes, R., do Amaral, L. N. R., Birky, J., Carone, L., Driscoll, P., Livesey, J. R., Graham, D., Becker, J., Cui, K., Schlecker, M., Garcia, R., Gialluca, M., Adams, A., Ahmed, MD. R., Bonney, P., Broussard, W., Chawla, C., Damasso, M., Danchi, W. C., ... Wojack, J. T. (2025). History and Habitability of the LP 890-9 Planetary System. Planetary Science Journal, 6(1), Article 25. https://doi.org/10.3847/PSJ/ad94dc

@article{da566e2a6cf245ff88825d94251d28bb,

title = "History and Habitability of the LP 890-9 Planetary System",

abstract = "We present numerous aspects of the evolution of the LP 890-9 (SPECULOOS-2/TOI-4306) planetary system, focusing on the likelihood that planet c can support life. We find that the host star reaches the main sequence in 1 Gyr and that planet c lies close to the inner boundary of the habitable zone. We find the magma ocean stage can last up to 50 Myr, remove eight Earth oceans of water, and leave up to 2000 bars of oxygen in the atmosphere. However, if the planet forms with a hydrogen envelope as small as 0.1 Earth masses, no water will be lost during the star's pre-main-sequence phase from thermal escape processes. We find that the planets are unlikely to be in a 3:1 mean motion resonance and that both planets tidally circularize within 0.5 Gyr when tidal dissipation is held constant. However, if tidal dissipation is a function of mantle temperature and rheology, then we find that planet c's orbit may require more than 7 Gyr to circularize, during which time tidal heating may reach hundreds of terawatts. We thus conclude that the habitability of planet c depends most strongly on the initial volatile content and internal properties, but no data yet preclude the viability of an active biosphere on the planet.",

author = "Rory Barnes and {do Amaral}, {Laura N.R.} and Jessica Birky and Ludmila Carone and Peter Driscoll and Livesey, {Joseph R.} and David Graham and Juliette Becker and Kaiming Cui and Martin Schlecker and Rodolfo Garcia and Megan Gialluca and Arthur Adams and Ahmed, {MD Redyan} and Paul Bonney and Wynter Broussard and Chetan Chawla and Mario Damasso and Danchi, {William C.} and Russell Deitrick and Elsa Ducrot and Fromont, {Emeline F.} and Gaches, {Brandt A.L.} and Sakshi Gupta and Hill, {Michelle L.} and Jackman, {James A.G.} and Janin, {Estelle M.} and Miko{\l}aj Karawacki and Koren, {Matheus Daniel} and Greca, {Roberto La} and Michaela Leung and Arturo Miranda-Rosete and Olohoy, {Michael Kent A.} and Cecelia Ngo and Daria Paul and Sahu, {Chandan Kumar} and Sarkar, {Debajyoti Basu} and Shadab, {Mohammad Afzal} and Schwieterman, {Edward W.} and Melissa Sedler and Katie Texeira and Allona Vazan and {Delgado Vega}, {Karen N.} and Rohit Vijayakumar and Wojack, {Jonathan T.}",

note = "Publisher Copyright: {\textcopyright} 2025. The Author(s). Published by the American Astronomical Society.",

year = "2025",

month = jan,

day = "1",

doi = "10.3847/PSJ/ad94dc",

language = "אנגלית",

volume = "6",

journal = "Planetary Science Journal",

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Barnes, R, do Amaral, LNR, Birky, J, Carone, L, Driscoll, P, Livesey, JR, Graham, D, Becker, J, Cui, K, Schlecker, M, Garcia, R, Gialluca, M, Adams, A, Ahmed, MDR, Bonney, P, Broussard, W, Chawla, C, Damasso, M, Danchi, WC, Deitrick, R, Ducrot, E, Fromont, EF, Gaches, BAL, Gupta, S, Hill, ML, Jackman, JAG, Janin, EM, Karawacki, M, Koren, MD, Greca, RL, Leung, M, Miranda-Rosete, A, Olohoy, MKA, Ngo, C, Paul, D, Sahu, CK, Sarkar, DB, Shadab, MA, Schwieterman, EW, Sedler, M, Texeira, K, Vazan, A, Delgado Vega, KN, Vijayakumar, R & Wojack, JT 2025, 'History and Habitability of the LP 890-9 Planetary System', Planetary Science Journal, vol. 6, no. 1, 25. https://doi.org/10.3847/PSJ/ad94dc

TY - JOUR

T1 - History and Habitability of the LP 890-9 Planetary System

AU - Barnes, Rory

AU - do Amaral, Laura N.R.

AU - Birky, Jessica

AU - Carone, Ludmila

AU - Driscoll, Peter

AU - Livesey, Joseph R.

AU - Graham, David

AU - Becker, Juliette

AU - Cui, Kaiming

AU - Schlecker, Martin

AU - Garcia, Rodolfo

AU - Gialluca, Megan

AU - Adams, Arthur

AU - Ahmed, MD Redyan

AU - Bonney, Paul

AU - Broussard, Wynter

AU - Chawla, Chetan

AU - Damasso, Mario

AU - Danchi, William C.

AU - Deitrick, Russell

AU - Ducrot, Elsa

AU - Fromont, Emeline F.

AU - Gaches, Brandt A.L.

AU - Gupta, Sakshi

AU - Hill, Michelle L.

AU - Jackman, James A.G.

AU - Janin, Estelle M.

AU - Karawacki, Mikołaj

AU - Koren, Matheus Daniel

AU - Greca, Roberto La

AU - Leung, Michaela

AU - Miranda-Rosete, Arturo

AU - Olohoy, Michael Kent A.

AU - Ngo, Cecelia

AU - Paul, Daria

AU - Sahu, Chandan Kumar

AU - Sarkar, Debajyoti Basu

AU - Shadab, Mohammad Afzal

AU - Schwieterman, Edward W.

AU - Sedler, Melissa

AU - Texeira, Katie

AU - Vazan, Allona

AU - Delgado Vega, Karen N.

AU - Vijayakumar, Rohit

AU - Wojack, Jonathan T.

PY - 2025/1/1

Y1 - 2025/1/1

N2 - We present numerous aspects of the evolution of the LP 890-9 (SPECULOOS-2/TOI-4306) planetary system, focusing on the likelihood that planet c can support life. We find that the host star reaches the main sequence in 1 Gyr and that planet c lies close to the inner boundary of the habitable zone. We find the magma ocean stage can last up to 50 Myr, remove eight Earth oceans of water, and leave up to 2000 bars of oxygen in the atmosphere. However, if the planet forms with a hydrogen envelope as small as 0.1 Earth masses, no water will be lost during the star's pre-main-sequence phase from thermal escape processes. We find that the planets are unlikely to be in a 3:1 mean motion resonance and that both planets tidally circularize within 0.5 Gyr when tidal dissipation is held constant. However, if tidal dissipation is a function of mantle temperature and rheology, then we find that planet c's orbit may require more than 7 Gyr to circularize, during which time tidal heating may reach hundreds of terawatts. We thus conclude that the habitability of planet c depends most strongly on the initial volatile content and internal properties, but no data yet preclude the viability of an active biosphere on the planet.

AB - We present numerous aspects of the evolution of the LP 890-9 (SPECULOOS-2/TOI-4306) planetary system, focusing on the likelihood that planet c can support life. We find that the host star reaches the main sequence in 1 Gyr and that planet c lies close to the inner boundary of the habitable zone. We find the magma ocean stage can last up to 50 Myr, remove eight Earth oceans of water, and leave up to 2000 bars of oxygen in the atmosphere. However, if the planet forms with a hydrogen envelope as small as 0.1 Earth masses, no water will be lost during the star's pre-main-sequence phase from thermal escape processes. We find that the planets are unlikely to be in a 3:1 mean motion resonance and that both planets tidally circularize within 0.5 Gyr when tidal dissipation is held constant. However, if tidal dissipation is a function of mantle temperature and rheology, then we find that planet c's orbit may require more than 7 Gyr to circularize, during which time tidal heating may reach hundreds of terawatts. We thus conclude that the habitability of planet c depends most strongly on the initial volatile content and internal properties, but no data yet preclude the viability of an active biosphere on the planet.

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DO - 10.3847/PSJ/ad94dc

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SN - 2632-3338

VL - 6

JO - Planetary Science Journal

JF - Planetary Science Journal

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ER -

History and Habitability of the LP 890-9 Planetary System

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