30 Arietis

30 Arietis (abbreviated 30 Ari) is a 6th-apparent-magnitude mulitple star system[4] in the constellation of Aries. 30 Arietis is the Flamsteed designation. 30 Arietis A and B are separated by 38.1″ or about 1,500 AU at a distance of 130 light years away. The main components of both systems are both binaries with a composite spectra belonging to F-type main-sequence stars, meaning they are fusing hydrogen in their cores. The 30 Arietis system is 910 million years old, one fifth the age of the Sun.

30 Arietis

30 Arietis star system hierarchy
Observation data
Epoch J2000      Equinox J2000
Constellation Aries
30 Arietis A
Right ascension 02h 37m 00.5235s[1]
Declination +24° 38′ 49.9880″[1]
Apparent magnitude (V)
30 Arietis B
Right ascension 02h 36m 57.7449s[2]
Declination +24° 38′ 53.0026″[2]
Apparent magnitude (V)
Characteristics
Spectral type F5 V / F6 V[3]
B−V color index 0.410 / 0.510[3]
Astrometry
30 Arietis A
Proper motion (μ) RA: 136.862±0.137[1] mas/yr
Dec.: −15.188±0.141[1] mas/yr
Parallax (π)22.1261 ± 0.0726[1] mas
Distance147.4 ± 0.5 ly
(45.2 ± 0.1 pc)
30 Arietis B
Proper motion (μ) RA: 141.411±0.083[2] mas/yr
Dec.: −10.677±0.086[2] mas/yr
Parallax (π)22.3641 ± 0.0516[2] mas
Distance145.8 ± 0.3 ly
(44.7 ± 0.1 pc)
Orbit[4][5]
Primary30 Arietis A
Companion30 Arietis BC
Period (P)34000 yr
Semi-major axis (a)40"
(1670 AU)
Orbit[5]
Primary30 Arietis B
Companion30 Arietis C
Period (P)80 yr
Semi-major axis (a)22.3 AU
Details
30 Arietis A
Mass1.31 ± 0.04[3] M☉
Radius1.37 ± 0.03[3] R☉
Age860±630[5] Myr
30 Arietis Ba
Mass1.16 ± 0.04[3] M☉
Radius1.13 ± 0.03[3] R☉
Age910±830[5] Myr
Other designations
CCDM 02370+2439, WDS 02370+2439

30 Arietis A
BD+24°376, HD 16246, HIP 12189, HR 765, SAO 75471

30 Arietis B
BD+24°375, HD 16232, HIP 12184, HR 764, SAO 75470
Database references
SIMBADA
B
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)

Star system

30 Arietis A and B are separated by 38.1", corresponding to 1,500 AU at a distance of 130 light years. The pair are at almost the same distance, have very similar proper motions, and are considered almost certain to be gravitationally bound with a likely period around 34,000 years.[5] The main components of both systems are both binaries with a composite spectra belonging to F-type main-sequence stars, meaning they are fusing hydrogen in their cores.[3]

30 Arietis A is a spectroscopic binary with an orbital period of 1.1 days.[6] The primary Aa is an F-type main sequence star about 31% more massive than the Sun, while the companion Ab is a faint red dwarf only about 15% the mass of the Sun.

30 Arietis B has been reported to have a red dwarf companion at a distance of 22 AU[5] and a likely giant exoplanet Bb at about 1 AU.[3] In 2020, after the inclination of the planetary orbit was measured, the "planet" was found to fall in the mass range of a brown or red dwarf.[7] The more distant companion was referred to as C to distinguish it from Bb, and at about 0.5" it has been imaged using adaptive optics.[5]

References
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  3. Guenther, E. W.; et al. (2009). "A substellar component orbiting the F-star 30 Arietis B". Astronomy and Astrophysics. 507 (3): 1659–1665. arXiv:0912.4619. Bibcode:2009A&A...507.1659G. doi:10.1051/0004-6361/200912112.
  4. Whitney Clavin (2015). "Planet 'Reared' by Four Parent Stars". NASA. Retrieved 4 March 2015.
  5. Roberts Jr, Lewis C.; Tokovinin, Andrei; Mason, Brian D.; Riddle, Reed L.; Hartkopf, William I.; Law, Nicholas M.; Baranec, Christoph (2015). "Know the Star, Know the Planet. III. Discovery of Late-Type Companions to Two Exoplanet Host Stars". The Astronomical Journal. 149 (4): 118. arXiv:1503.01211. Bibcode:2015AJ....149..118R. doi:10.1088/0004-6256/149/4/118. S2CID 30908636.
  6. Morbey, C. L.; Brosterhus, E. B. (1974). "A Search for Spectroscopic Binaries from Published Radial Velocity Data". Publications of the Astronomical Society of the Pacific. 86 (512): 455. Bibcode:1974PASP...86..455M. doi:10.1086/129630. JSTOR 40675565.
  7. Kiefer, Flavien; Hébrard, Guillaume; Lecavelier, Alain; Martioli, Eder; Dalal, Shweta; Vidal-Madjar, Alfred (2021). "Determining the true mass of radial-velocity exoplanets with Gaia 9 planet candidates in the brown-dwarf/stellar regime and 27 confirmed planets". Astronomy & Astrophysics. A7: 645. arXiv:2009.14164. doi:10.1051/0004-6361/202039168. S2CID 221995447.

This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.