GJ 1151

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GJ 1151
GJ 1151 + GJ 1151 b.png
Artist's impression of GJ 1151 and an orbiting planet
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Ursa Major
Right ascension 11h 50m 57.72053s [1]
Declination +48° 22′ 38.5612″ [1]
Apparent magnitude  (V)14.008 [2]
Characteristics
Spectral type dM4.5 [2]
B−V color index 1.787 [3]
Astrometry
Radial velocity (Rv)−36.13±0.26 [1]  km/s
Proper motion (μ)RA: -1545.069  mas/yr [1]
Dec.: -962.724  mas/yr [1]
Parallax (π)124.3378 ± 0.0549  mas [1]
Distance 26.23 ± 0.01  ly
(8.043 ± 0.004  pc)
Absolute magnitude  (MV)14.482±0.022 [2]
Details
Mass 0.1639±0.0093 [4]   M☉
Radius 0.1781±0.0042 [4]   R☉
Luminosity (bolometric)0.003315±0.000018 [4]   L☉
Surface gravity (log g)5.09±0.09 [4]   cgs
Temperature 3,143±26 [2]   K
Metallicity [Fe/H]−0.12±0.10 [4]   dex
Rotation 140±10  d
Rotational velocity (v sin i)2.0 [5]  km/s
Age 2.5 [3]   Gyr
Other designations
GJ  1151, G 122-49, LHS  316, NLTT  28752, 2MASS J11505787+4822395, Gaia EDR3 786834302080370304 [6]
Database references
SIMBAD data

GJ 1151 is a star located in the northern circumpolar constellation of Ursa Major at a distance of 26.2 light-years (8.0 parsecs ) from the Sun. It has a reddish hue and is too faint to be visible to the naked eye with an apparent visual magnitude of 14.0 [2] The star is moving closer with a radial velocity of −36 km/s, [5] and has a relatively large proper motion, traversing the celestial sphere at a rate of 1.815″ ·yr−1. [7]

Contents

This is a small red dwarf star of spectral type dM4.5. [2] It is 2.5 [3]  billion years old and is spinning with a projected rotational velocity of 2.0 km/s. [5] The star has 15.4% [3] of the mass of the Sun and 19.0% [3] of the Sun's radius, with an effective temperature of 3,143 K. [2]

Planetary system

In 2020, astronomers announced the discovery of radio emissions from the star which are consistent with the star having a magnetic interaction with a planet approximately the size of Earth, revolving in a 1-5 day long orbit. [8] [9] [10] [11] [12] [13] Such an interaction would be analogous to a scaled-up version of the Jupiter-Io magnetic interaction, with GJ 1151 taking the role of Jupiter and its planet the role of Io.

Two papers published only a month apart in 2021 discussed planet detection at GJ 1151 by the radial velocity method. One claimed the detection of a planet with a minimum mass of 2.5  M🜨 and a period of 2 days, supporting the radio emission detection, [14] while the other was unable to confirm this candidate planet, finding that the 2-day signal is likely caused by long-term variability, possibly connected to a more distant planet. [15] This second study placed an upper limit of 0.7-1.2 M🜨 on the minimum masses of any undetected planets with periods from 1-5 days. [15]

In 2023, a different planet was found, with a minimum mass of 10.6 M🜨 and a 390-day orbit, along with additional radial velocity variations. This new planet was referred to by the preprint version of the discovery paper as GJ 1151 b, but the published version of the paper, as well as the NASA Exoplanet Archive, refer to it as GJ 1151 c to differentiate it from the previous candidate. While the presence of a short-period planet associated with the radio emissions could not be completely ruled out, if such a planet exists its minimum mass must be less than 1.2 M🜨. [4]

The GJ 1151 planetary system [4]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
c≥10.62+1.31
−1.47  M🜨 		0.5714+0.0053
−0.0064		389.7+5.4
−6.5		———

See also

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References

  1. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics . arXiv: 2208.00211 . doi: 10.1051/0004-6361/202243940 . Gaia DR3 record for this source at VizieR.
  2. 1 2 3 4 5 6 7 Houdebine, Éric R.; et al. (August 2019). "The Mass-Activity Relationships in M and K Dwarfs. I. Stellar Parameters of Our Sample of M and K Dwarfs". The Astronomical Journal. 158 (2): 17. arXiv: 1905.07921 . Bibcode:2019AJ....158...56H. doi: 10.3847/1538-3881/ab23fe . S2CID   159041104. 56.
  3. 1 2 3 4 5 Mann, Andrew W.; et al. (May 2015). "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius". The Astrophysical Journal. 804 (1): 38. arXiv: 1501.01635 . Bibcode:2015ApJ...804...64M. doi:10.1088/0004-637X/804/1/64. S2CID   19269312. 64.
  4. 1 2 3 4 5 6 7 Blanco-Pozo, J.; Perger, M.; et al. (March 2023). "The CARMENES search for exoplanets around M dwarfs. A long-period planet around GJ 1151 measured with CARMENES and HARPS-N data". Astronomy & Astrophysics . 671: A50. arXiv: 2301.04442 . Bibcode:2023A&A...671A..50B. doi:10.1051/0004-6361/202245053.
  5. 1 2 3 Jeffers, S. V.; et al. (June 2018). "CARMENES input catalogue of M dwarfs. III. Rotation and activity from high-resolution spectroscopic observations". Astronomy & Astrophysics. 614: 19. arXiv: 1802.02102 . Bibcode:2018A&A...614A..76J. doi:10.1051/0004-6361/201629599. S2CID   56147445. A76.
  6. ↑ "G 122-49". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-03-02.
  7. ↑ Lépine, Sébastien; Shara, Michael M. (March 2005). "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)". The Astronomical Journal. 129 (3): 1483–1522. arXiv: astro-ph/0412070 . Bibcode:2005AJ....129.1483L. doi:10.1086/427854. S2CID   2603568.
  8. ↑ Vedantham, H. K.; et al. (2020-02-17). "Coherent radio emission from a quiescent red dwarf indicative of star–planet interaction". Nature Astronomy . 4 (6): 577–583. arXiv: 2002.08727 . Bibcode:2020NatAs...4..577V. doi:10.1038/s41550-020-1011-9. hdl:1887/3133600. ISSN   2397-3366. S2CID   211204712.
  9. ↑ Pope, Benjamin J. S.; et al. (17 February 2020). "No Massive Companion to the Coherent Radio-emitting M Dwarf GJ 1151". The Astrophysical Journal Letters . 890 (2): L19. arXiv: 2002.07850 . Bibcode:2020ApJ...890L..19P. doi: 10.3847/2041-8213/ab5b99 . S2CID   211171765.
  10. ↑ Starr, Michelle (29 February 2020). "For The First Time, Astronomers Have Detected an Exoplanet Using Radio Waves". ScienceAlert.com. Retrieved 1 March 2020.
  11. ↑ "Radio telescope measures aurorae in distant planetary system". UPI. Retrieved 2020-02-26.
  12. ↑ Redd, Nola Taylor (18 February 2020). "New Exoplanet Search Strategy Claims First Discovery". Quanta Magazine. Retrieved 2020-02-26.
  13. ↑ Clark, Stuart. "An exoplanet is generating radio waves from its red dwarf sun". New Scientist. Retrieved 2020-02-26.
  14. ↑ Mahadevan, Suvrath; Stefánsson, Gudmundur; Robertson, Paul; Terrien, Ryan C.; Ninan, Joe P.; Holcomb, Rae J.; Halverson, Samuel; Cochran, William D.; Kanodia, Shubham; Ramsey, Lawrence W.; Wolszczan, Alexander; Endl, Michael; Bender, Chad F.; Diddams, Scott A.; Fredrick, Connor; Hearty, Fred; Monson, Andrew; Metcalf, Andrew J.; Roy, Arpita; Schwab, Christian (2021), "The Habitable-zone Planet Finder Detects a Terrestrial-mass Planet Candidate Closely Orbiting Gliese 1151: The Likely Source of Coherent Low-frequency Radio Emission from an Inactive Star", The Astrophysical Journal Letters, 919 (1): L9, arXiv: 2102.02233 , Bibcode:2021ApJ...919L...9M, doi: 10.3847/2041-8213/abe2b2 , S2CID   231802021
  15. 1 2 Perger, M.; Ribas, I.; Anglada-Escudé, G.; Morales, J. C.; Amado, P. J.; Caballero, J. A.; Quirrenbach, A.; Reiners, A.; Béjar, V. J. S.; Dreizler, S.; Galadí-Enríquez, D.; Hatzes, A. P.; Henning, Th.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Lafarga, M.; Montes, D.; Pallé, E.; Rodríguez-López, C.; Schweitzer, A.; Zapatero Osorio, M. R.; Zechmeister, M. (2021), "The CARMENES search for exoplanets around M dwarfs", Astronomy & Astrophysics, 649: L12, arXiv: 2103.10216 , Bibcode:2021A&A...649L..12P, doi:10.1051/0004-6361/202140786, S2CID   126038821
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