TESS Discovery of an Ultra-short-period Planet around the Nearby M Dwarf LHS 3844

Vanderspek, Roland and Huang, Chelsea X. ORCID: https://orcid.org/0000-0003-0918-7484 and Vanderburg, Andrew and Ricker, George R. and Latham, David W. and Seager, Sara and Winn, Joshua N. and Jenkins, Jon M. and Burt, Jennifer and Dittmann, Jason and Newton, Elisabeth and Quinn, Samuel N. and Shporer, Avi and Charbonneau, David and Irwin, Jonathan and Ment, Kristo and Winters, Jennifer G. and Collins, Karen A. and Evans, Phil and Gan, Tianjun and Hart, Rhodes and Jensen, Eric L. N. and Kielkopf, John and Mao, Shude and Waalkes, William and Bouchy, Francois and Marmier, Maxime and Nielsen, Louise D. and Ottoni, Gael and Pepe, Francesco and Segransan, Damien and Udry, Stephane and Henry, Todd and Paredes, Leonardo A. and James, Hodari-Sadiki and Hinojosa, Rodrigo H. and Silverstein, Michele L. and Palle, Enric and Berta-Thompson, Zachory and Crossfield, Ian and Davies, Misty D. and Dragomir, Diana and Fausnaugh, Michael and Glidden, Ana and Pepper, Joshua and Morgan, Edward H. and Rose, Mark and Twicken, Joseph D. and Villasenor, Jesus Noel S. and Yu, Liang and Bakos, Gaspar and Bean, Jacob and Buchhave, Lars A. and Christensen-Dalsgaard, Jorgen and Christiansen, Jessie L. and Ciardi, David R. and Clampin, Mark and De Lee, Nathan and Deming, Drake and Doty, John and Jernigan, J. Garrett and Kaltenegger, Lisa and Lissauer, Jack J. and McCullough, P. R. and Narita, Norio and Paegert, Martin and Pal, Andras and Rinehart, Stephen and Sasselov, Dimitar and Sato, Bunei and Sozzetti, Alessandro and Stassun, Keivan G. and Torres, Guillermo (2019) TESS Discovery of an Ultra-short-period Planet around the Nearby M Dwarf LHS 3844. The Astrophysical Journal Letters, 871 (2):L24. pp. 1-9. ISSN 2041-8205

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Abstract

Data from the newly commissioned Transiting Exoplanet Survey Satellite has revealed a 'hot Earth' around LHS 3844, an M dwarf located 15 pc away. The planet has a radius of R ⊕ and orbits the star every 11 hr. Although the existence of an atmosphere around such a strongly irradiated planet is questionable, the star is bright enough (I = 11.9, K = 9.1) for this possibility to be investigated with transit and occultation spectroscopy. The star's brightness and the planet's short period will also facilitate the measurement of the planet's mass through Doppler spectroscopy.


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Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Additional Information: Published version deposited in accordance with the copyright policy of the publisher.
Faculty/School / Institute/Centre: Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -)
Faculty/School / Institute/Centre: Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -)
Date Deposited: 31 Mar 2022 04:30
Last Modified: 17 May 2022 03:32
Uncontrolled Keywords: planetary systems; planets and satellites: detection; stars: individual (LHS 3844, TIC 410153553); Astrophysics - Earth and Planetary Astrophysics
Fields of Research (2020): 51 PHYSICAL SCIENCES > 5101 Astronomical sciences > 510109 Stellar astronomy and planetary systems
Identification Number or DOI: https://doi.org/10.3847/2041-8213/aafb7a
URI: http://eprints.usq.edu.au/id/eprint/47374

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