Gliese 433
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Hydra
Right ascension 11h 35m 26.94777s[1]
Declination −32° 32′ 23.8842″[1]
Apparent magnitude (V) 9.81[2]
Characteristics
Spectral type M2V[3]
Apparent magnitude (U) 12.508[2]
Apparent magnitude (B) 11.299[2]
Apparent magnitude (R) 8.82[2]
Apparent magnitude (I) 7.664[2]
Apparent magnitude (J) 6.471[2]
Apparent magnitude (H) 5.856±0.036[2]
Apparent magnitude (K) 5.623±0.021[2]
U−B color index 1.23[2]
B−V color index 1.489±0.004[2]
V−R color index 0.99[2]
R−I color index 1.16[2]
Astrometry
Radial velocity (Rv)+17.986±0.0006[4] km/s
Proper motion (μ) RA: −71.060±0.020 mas/yr[1]
Dec.: −850.592±0.016 mas/yr[1]
Parallax (π)110.1711 ± 0.0204 mas[1]
Distance29.605 ± 0.005 ly
(9.077 ± 0.002 pc)
Absolute magnitude (MV)10.07[2]
Details
Mass0.48[5] M☉
Radius0.529±0.021[6] R☉
Luminosity0.034[7] L☉
Habitable zone inner limit0.186 AU[8]
Habitable zone outer limit0.362 AU[8]
Surface gravity (log g)4.81±0.14[9] cgs
Temperature3,445±50[6] K
Metallicity [Fe/H]−0.02±0.05[10] dex
Rotation73.2±16.0 d[11]
Rotational velocity (v sin i)1.0[6] km/s
Other designations
CD−31 9113, GJ 433, HIP 56528, SAO 202602, LHS 2429, LTT 4290, NLTT 27914, 2MASS J11352695-3232232
Database references
SIMBADdata
Exoplanet Archivedata
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)

Gliese 433 is a dim red dwarf star with multiple exoplanetary companions, located in the equatorial constellation of Hydra. The system is located at a distance of 29.6 light-years from the Sun based on parallax measurements, and it is receding with a radial velocity of +18 km/s.[4] Based on its motion through space, this is an old disk star.[7] It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 9.81[2] and an absolute magnitude of 10.07.[2]

This is a small M-type main-sequence star with a stellar classification of M2V.[3] It is an older star[12] with a rotation period of roughly 73 days[11] and a below average activity level for stars of its mass.[7] The star has 48%[5] of the mass and 53%[6] of the radius of the Sun. It is radiating just 3.4%[7] of the luminosity of the Sun from its photosphere at an effective temperature of 3,445 K.[6]

Planetary system

Gliese 433 b is an extrasolar planet which orbits the star Gliese 433. This planet is a super-Earth with at least six times the mass of Earth and takes approximately seven days to orbit the star at a semimajor axis of approximately 0.056 AU. The planet was announced in a press release in October 2009, but no discovery paper at the time was made available.[13] A study described in a 2014 paper by Tuomi et al. confirmed both Gliese 433 b and another candidate planet, previously detected in 2012, Gliese 433 c.[14]

Gliese 433 d, whose discovery was published in January 2020, is similar in mass to Gliese 433 b but orbits slightly further out, actually within the optimistic habitable zone of the star, but it is still too close to the star, and therefore too warm, to be inside the narrower boundaries of the conservative habitable zone.[8][15]

Gliese 433 c orbits the furthest out from the star. As of 2020 it is the nearest, widest orbiting, and coldest Neptune-like planet yet detected. It is also notable in having an unusually eccentric orbit for a large planet so far from its parent single star and other planets.[15]

A survey using the Herschel Telescope found an infrared excess around the star, indicating the presence of an orbiting circumstellar disk. This feature is unresolved but the mean temperature of 30 K puts it somewhere within a 16 AU radius from the host star.[12]

The Gliese 433 planetary system[15]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥6.043±0.597 M🜨 0.062±0.002 7.3705±0.0005 0.04±0.03 — —
d ≥5.223±0.921 M🜨 0.178±0.006 36.059±0.016 0.07±0.05 — —
c ≥32.422±6.329 M🜨 4.819±0.417 5,094.105±608.617 0.12±0.07 — —

See also

References

  1. ^ a b c d 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.
  2. ^ a b c d e f g h i j k l m n o Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  3. ^ a b Henry, Todd J.; et al. (2002). "The Solar Neighborhood. VI. New Southern Nearby Stars Identified by Optical Spectroscopy". The Astronomical Journal. 123 (4): 2002–2009. arXiv:astro-ph/0112496. Bibcode:2002AJ....123.2002H. doi:10.1086/339315. ISSN 0004-6256. S2CID 17735847.
  4. ^ a b Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv:1804.09370. Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID 52952408.
  5. ^ a b Zechmeister, M.; et al. (August 6, 2009). "The M dwarf planet search programme at the ESO VLT + UVES. A search for terrestrial planets in the habitable zone of M dwarfs". Astronomy and Astrophysics. 505 (2): 859–871. arXiv:0908.0944. Bibcode:2009A&A...505..859Z. doi:10.1051/0004-6361/200912479. S2CID 16845441.
  6. ^ a b c d e Houdebine, E. R. (September 2010). "Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars". Monthly Notices of the Royal Astronomical Society. 407 (3): 1657–1673. Bibcode:2010MNRAS.407.1657H. doi:10.1111/j.1365-2966.2010.16827.x.
  7. ^ a b c d Delfosse, X.; et al. (May 2013). "The HARPS search for southern extra-solar planets. XXXIII. Super-Earths around the M-dwarf neighbors Gl 433 and Gl 667C". Astronomy & Astrophysics. 553: 15. arXiv:1202.2467. Bibcode:2013A&A...553A...8D. doi:10.1051/0004-6361/201219013. S2CID 119270684. A8.
  8. ^ a b c "PHL's Exoplanets Catalog". University of Puerto Rico at Arecibo. 5 December 2019. Archived from the original on 21 May 2019. Retrieved 26 January 2020.
  9. ^ Stassun, Keivan G.; et al. (2016). "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes". The Astronomical Journal. 153 (3): 136. arXiv:1609.04389. Bibcode:2017AJ....153..136S. doi:10.3847/1538-3881/aa5df3. S2CID 119219062.
  10. ^ Lindgren, Sara; Heiter, Ulrike (2017). "Metallicity determination of M dwarfs. Expanded parameter range in metallicity and effective temperature". Astronomy and Astrophysics. 604: A97. arXiv:1705.08785. Bibcode:2017A&A...604A..97L. doi:10.1051/0004-6361/201730715. S2CID 119216828.
  11. ^ a b Suárez Mascareño, A.; et al. (September 2015). "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators". Monthly Notices of the Royal Astronomical Society. 452 (3): 2745–2756. arXiv:1506.08039. Bibcode:2015MNRAS.452.2745S. doi:10.1093/mnras/stv1441. S2CID 119181646.
  12. ^ a b Kennedy, G. M.; et al. (June 2018). "Kuiper belt analogues in nearby M-type planet-host systems". Monthly Notices of the Royal Astronomical Society. 476 (4): 4584–4591. arXiv:1803.02832. Bibcode:2018MNRAS.476.4584K. doi:10.1093/mnras/sty492.
  13. ^ "32 New Exoplanets Found". ESO News. ESO. Retrieved 15 February 2012.
  14. ^ Tuomi, Mikko; Jones, Hugh R. A.; Barnes, John R.; et al. (2014). "Bayesian search for low-mass planets around nearby M dwarfs – estimates for occurrence rate based on global detectability statistics". Monthly Notices of the Royal Astronomical Society. 441 (2): 1545–1569. arXiv:1403.0430. Bibcode:2014MNRAS.441.1545T. doi:10.1093/mnras/stu358. ISSN 1365-2966.
  15. ^ a b c Feng, Fabo; Butler, R. Paul; Shectman, Stephen A.; et al. (2020). "Search for Nearby Earth Analogs. II. Detection of Five New Planets, Eight Planet Candidates, and Confirmation of Three Planets around Nine Nearby M Dwarfs". The Astrophysical Journal Supplement Series. 246 (1): 38. arXiv:2001.02577. Bibcode:2020ApJS..246...11F. doi:10.3847/1538-4365/ab5e7c. ISSN 1538-4365. S2CID 210064560. 11.


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