A giant planet transiting a 3-Myr protostar with a misaligned disk

Barber, Madyson G.; Mann, Andrew W.; Vanderburg, Andrew; Krolikowski, Daniel; Kraus, Adam; Ansdell, Megan; Pearce, Logan; Mace, Gregory N.; Andrews, Sean M.; Boyle, Andrew W.; Collins, Karen A.; Furio, Matthew; Dragomir, Diana; Espaillat, Catherine; Feinstein, Adina D.; Fields, Matthew; Jaffe, Daniel; Murillo, Ana Isabel Lopez; Murgas, Felipe; Newton, Elisabeth R.; Palle, Enric; Sawczynec, Erica; Schwarz, Richard P.; Thao, Pa Chia; Tofflemire, Benjamin M.; Watkins, Cristilyn N.; Jenkins, Jon M.; Latham, David W.; Ricker, George; Seager, Sara; Vanderspek, Roland; Winn, Joshua N.; Charbonneau, David; Essack, Zahra; Rodriguez, David R.; Shporer, Avi; Twicken, Joseph D.; Villaseñor, Jesus Noel

A giant planet transiting a 3-Myr protostar with a misaligned disk

Madyson G. Barber (), Andrew W. Mann, Andrew Vanderburg, Daniel Krolikowski, Adam Kraus, Megan Ansdell, Logan Pearce, Gregory N. Mace, Sean M. Andrews, Andrew W. Boyle, Karen A. Collins, Matthew Furio, Diana Dragomir, Catherine Espaillat, Adina D. Feinstein, Matthew Fields, Daniel Jaffe, Ana Isabel Lopez Murillo, Felipe Murgas, Elisabeth R. Newton, Enric Palle, Erica Sawczynec, Richard P. Schwarz, Pa Chia Thao, Benjamin M. Tofflemire, Cristilyn N. Watkins, Jon M. Jenkins, David W. Latham, George Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn, David Charbonneau, Zahra Essack, David R. Rodriguez, Avi Shporer, Joseph D. Twicken and Jesus Noel Villaseñor
Additional contact information
Madyson G. Barber: University of North Carolina at Chapel Hill
Andrew W. Mann: University of North Carolina at Chapel Hill
Andrew Vanderburg: Massachusetts Institute of Technology
Daniel Krolikowski: The University of Arizona
Adam Kraus: The University of Texas at Austin
Megan Ansdell: NASA Headquarters
Logan Pearce: The University of Arizona
Gregory N. Mace: The University of Texas at Austin
Sean M. Andrews: Center for Astrophysics ∣ Harvard & Smithsonian
Andrew W. Boyle: University of North Carolina at Chapel Hill
Karen A. Collins: Center for Astrophysics ∣ Harvard & Smithsonian
Matthew Furio: The University of Texas at Austin
Diana Dragomir: The University of New Mexico
Catherine Espaillat: Boston University
Adina D. Feinstein: University of Colorado Boulder
Matthew Fields: University of North Carolina at Chapel Hill
Daniel Jaffe: The University of Texas at Austin
Ana Isabel Lopez Murillo: University of North Carolina at Chapel Hill
Felipe Murgas: Instituto de Astrofísica de Canarias (IAC)
Elisabeth R. Newton: Dartmouth College
Enric Palle: Instituto de Astrofísica de Canarias (IAC)
Erica Sawczynec: The University of Texas at Austin
Richard P. Schwarz: Center for Astrophysics ∣ Harvard & Smithsonian
Pa Chia Thao: University of North Carolina at Chapel Hill
Benjamin M. Tofflemire: The University of Texas at Austin
Cristilyn N. Watkins: Center for Astrophysics ∣ Harvard & Smithsonian
Jon M. Jenkins: NASA Ames Research Center
David W. Latham: Center for Astrophysics ∣ Harvard & Smithsonian
George Ricker: Massachusetts Institute of Technology
Sara Seager: Massachusetts Institute of Technology
Roland Vanderspek: Massachusetts Institute of Technology
Joshua N. Winn: Princeton University
David Charbonneau: Center for Astrophysics ∣ Harvard & Smithsonian
Zahra Essack: The University of New Mexico
David R. Rodriguez: Space Telescope Science Institute
Avi Shporer: Massachusetts Institute of Technology
Joseph D. Twicken: NASA Ames Research Center
Jesus Noel Villaseñor: Massachusetts Institute of Technology

Nature, 2024, vol. 635, issue 8039, 574-577

Abstract: Abstract Astronomers have found more than a dozen planets transiting stars that are 10–40 million years old1, but younger transiting planets have remained elusive. The lack of such discoveries may be because planets have not fully formed at this age or because our view is blocked by the protoplanetary disk. However, we now know that many outer disks are warped or broken2; provided the inner disk is depleted, transiting planets may thus be visible. Here we report observations of the transiting planet IRAS 04125+2902 b orbiting a 3-million-year-old, 0.7-solar-mass, pre-main-sequence star in the Taurus Molecular Cloud. The host star harbours a nearly face-on (30 degrees inclination) transitional disk3 and a wide binary companion. The planet has a period of 8.83 days, a radius of 10.7 Earth radii (0.96 Jupiter radii) and a 95%-confidence upper limit on its mass of 90 Earth masses (0.3 Jupiter masses) from radial-velocity measurements, making it a possible precursor of the super-Earths and sub-Neptunes frequently found around main-sequence stars. The rotational broadening of the star and the orbit of the wide (4 arcseconds, 635 astronomical units) companion are both consistent with edge-on orientations. Thus, all components of the system are consistent with alignment except the outer disk; the origin of this misalignment is unclear.

Date: 2024
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DOI: 10.1038/s41586-024-08123-3

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