K2-3

Last updated
K2-3
Observation data
Epoch J2000       Equinox J2000
Constellation Leo [1]
Right ascension 11h 29m 20.39171s [2]
Declination −01° 27′ 17.2817″ [2]
Apparent magnitude  (V)12.168±0.009 [3]
Characteristics
Spectral type M0V [4]
B−V color index 1.35 ± 0.06 [4]
Astrometry
Radial velocity (Rv)30.24±0.46 [2]  km/s
Proper motion (μ)RA: 94.116  mas/yr [2]
Dec.: −78.003  mas/yr [2]
Parallax (π)22.7374 ± 0.0220  mas [2]
Distance 143.4 ± 0.1  ly
(43.98 ± 0.04  pc)
Details [5]
Mass 0.549+0.029
−0.027  M☉
Radius 0.546+0.018
−0.016  R☉
Luminosity (bolometric)0.0587+0.0018
−0.0019  L☉
Surface gravity (log g)4.704+0.023
−0.026  cgs
Temperature 3844+61
−63  K
Metallicity [Fe/H]−0.157+0.075
−0.080  dex
Rotation 40±2 d [6]
Age 6.9±4.7  Gyr
Other designations
Gaia DR3  3796690380302214272, EPIC  201367065, 2MASS J11292037-0127173, WISE J112920.45-012718.0 [7]
Database references
SIMBAD data

K2-3, also known as EPIC 201367065, [4] is a red dwarf star with three known planets. It is on the borderline of being a late orange dwarf/K-type star, but because of its temperature, it is classified as a red dwarf (4,000 K is typically the division line between spectral class M and K).

At a distance of 143 light-years (44 parsecs ), [2] the star's proximity means it is bright enough to make it feasible for astronomers to study the planets' atmospheres to determine whether they are like Earth's atmosphere and possibly conducive to life.

Planetary system

K2-3 has three confirmed exoplanets, discovered in 2015. [8] All are low-density super-Earths or sub-Neptunes, with the outermost orbiting near the inner edge of the habitable zone. [9] [5]

The K2-3 planetary system [5] [10]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 5.11+0.65
−0.64  M🜨 		0.0778±0.002610.054626(0)<0.09489.588+0.12
−0.100 ° 		2.078+0.076
−0.067  R🜨
c 2.68±0.85  M🜨 0.1414±0.004724.646582(39)<0.09589.905+0.066
−0.088 ° 		1.582+0.057
−0.051  R🜨
d <1.6  M🜨 0.2097±0.007044.556456(97)<0.09789.788+0.033
−0.029 ° 		1.458+0.056
−0.051  R🜨

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<span class="mw-page-title-main">WASP-4</span> G-type main sequence star in the constellation Phoenix

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<span class="mw-page-title-main">K2-3d</span> Mini-Neptune orbiting K2-3

K2-3d, also known as EPIC 201367065 d, is a confirmed exoplanet of probable mini-Neptune type orbiting the red dwarf star K2-3, and the outermost of three such planets discovered in the system. It is located 143 light-years away from Earth in the constellation of Leo. The exoplanet was found by using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. It was the first planet in the Kepler "Second Light" mission to receive the letter "d" designation for a planet. Its discovery was announced in January 2015.

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K2-19 is an early K-type or late G-type main sequence star that is magnetically active, and has a light curve that exhibits variations in brightness of ~1%. It is located approximately 976 light-years away in the constellation Virgo. Three confirmed transiting exoplanets are known to orbit this star.

<span class="mw-page-title-main">K2-18</span> Red dwarf star in the constellation Leo

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L 98-59 is a bright M dwarf star, located in the constellation of Volans, at a distance of 10.608 parsecs, as measured by Gaia.

<span class="mw-page-title-main">K2-25</span>

K2-25 is a young red dwarf star located in the Hyades cluster. There is a single known Neptune-sized planet in a 3.5 day orbit.

References

  1. ↑ Roman, Nancy G. (1987). "Identification of a Constellation From a Position". Publications of the Astronomical Society of the Pacific. 99 (617): 695–699. Bibcode:1987PASP...99..695R. doi: 10.1086/132034 . Vizier query form
  2. 1 2 3 4 5 6 7 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  3. ↑ Henden, A. A.; et al. (2016). "VizieR Online Data Catalog: AAVSO Photometric All Sky Survey (APASS) DR9 (Henden+, 2016)". VizieR On-line Data Catalog: II/336. Originally Published in: 2015AAS...22533616H. 2336. Bibcode:2016yCat.2336....0H. Vizier catalog entry
  4. 1 2 3 "K2-3 PLANET HOST OVERVIEW PAGE". NASA Exoplanet Archive. Retrieved 2015-10-17.
  5. 1 2 3 Diamond-Lowe, Hannah; et al. (2022), "The K2-3 System Revisited: Testing Photoevaporation and Core-powered Mass Loss with Three Small Planets Spanning the Radius Valley", The Astronomical Journal, 164 (5): 172, arXiv: 2207.12755 , Bibcode:2022AJ....164..172D, doi: 10.3847/1538-3881/ac7807 , S2CID   251067119
  6. ↑ Kosiarek, Molly R.; et al. (2019). "Bright Opportunities for Atmospheric Characterization of Small Planets: Masses and Radii of K2-3 b, c, and d and GJ3470 b from Radial Velocity Measurements and Spitzer Transits". The Astronomical Journal. 157 (3) 97. arXiv: 1812.08241 . Bibcode: 2019AJ....157...97K . doi: 10.3847/1538-3881/aaf79c . S2CID   119440420.
  7. ↑ "K2-3". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2024-04-19.
  8. ↑ Crossfield, Ian J. M.; et al. (2015). "A Nearby M Star with Three Transiting Super-Earths Discovered by K2". The Astrophysical Journal. 804 (1) 10. arXiv: 1501.03798 . Bibcode: 2015ApJ...804...10C . doi: 10.1088/0004-637X/804/1/10 .
  9. ↑ Damasso, Mario; et al. (2018). "Eyes on K2-3: A system of three likely sub-Neptunes characterized with HARPS-N and HARPS". Astronomy and Astrophysics. 615 A69. arXiv: 1802.08320 . Bibcode: 2018A&A...615A..69D . doi: 10.1051/0004-6361/201732459 . S2CID   58923147.
  10. ↑ Bonomo, A. S.; Dumusque, X.; et al. (April 2023). "Cold Jupiters and improved masses in 38 Kepler and K2 small-planet systems from 3661 high-precision HARPS-N radial velocities. No excess of cold Jupiters in small-planet systems". Astronomy & Astrophysics . arXiv: 2304.05773 . doi:10.1051/0004-6361/202346211. S2CID   261556620.
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