Astronomy:HD 142

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Short description: Wide binary star system in the constellation Phoenix
HD 142
Observation data
{{#ifeq:J2000.0|J2000.0 (ICRS)|Epoch J2000.0      Equinox J2000.0 (ICRS)| Epoch J2000.0      [[Astronomy:Equinox (celestial coordinates)|Equinox J2000.0}}
Constellation Phoenix[1]
HD 142 A
Right ascension  00h 06m 19.1754s[2]
Declination –49° 04′ 30.6741″[2]
Apparent magnitude (V) 5.711±0.003[3]
HD 142 B
Right ascension  00h 06m 19.1480s[4]
Declination –49° 04′ 34.9177″[4]
Apparent magnitude (V) +11.5[5]
Characteristics
Evolutionary stage main sequence
Spectral type F7V[6] + K8.5-M1.5[7]
B−V color index 0.519±0.011[8]
Astrometry
HD 142 A
Radial velocity (Rv)5.76±0.12[9] km/s
Proper motion (μ) RA: 575.099±0.017[9] mas/yr
Dec.: −40.874±0.024[9] mas/yr
Parallax (π)38.1945 ± 0.0355[9] mas
Distance85.39 ± 0.08 ly
(26.18 ± 0.02 pc)
Absolute magnitude (MV)3.66±0.02[10]
HD 142 B
Proper motion (μ) RA: 566.984±0.023[11] mas/yr
Dec.: −17.387±0.027[11] mas/yr
Parallax (π)38.2306 ± 0.0349[11] mas
Distance85.31 ± 0.08 ly
(26.16 ± 0.02 pc)
Details[12]
HD 142 A
Mass1.25±0.10 M☉
Radius1.41±0.11 R☉
Luminosity2.9 L☉
Surface gravity (log g)4.34±0.14 cgs
Temperature6,338±46 K
Metallicity [Fe/H]0.03±0.04 dex
Rotational velocity (v sin i)9.58±0.74[13] km/s
Age2.5 Gyr
HD 142 B
Mass0.54[14] M☉
Other designations
HD 142A: CD−49°14337, HD 142, HIP 522, HR 6, SAO 214963, WDS J00063-4905A[15]
HD 142B: CD−49°14337B, WDS J00063-4905B, NLTT 218, 2MASS J00061919-4904348[16]
Database references
SIMBADdata

HD 142 is a wide binary star[5] system in the southern constellation of Phoenix. The main component has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.7.[3] The system is located at a distance of 85.5 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of +6 km/s.[17]

The primary component is an F-type main-sequence star with a stellar classification of F7V,[6] which indicates it is undergoing core hydrogen fusion. It is an estimated 2.5[12] billion years old and is spinning with a projected rotational velocity of 10 km/s.[13] The star has 1.25 times the mass of the Sun and 1.4 times the Sun's radius. It is radiating 2.9 times the luminosity of the Sun from its photosphere at an effective temperature of 6,338 K.[12]

A magnitude 11.5[5] companion star was detected in 1894 making this a binary star system.[18] The binary companion was confirmed to be gravitationally bound in 2007 and determined to be a red dwarf of spectral type K8.5-M1.5[7] with 54% of the Sun's mass.[14] The pair have a projected separation of 120.6 astronomical unit|AU.[14]


Planetary system

In 2001, the Anglo-Australian Planet Search team led by Chris Tinney announced the discovery of an extrasolar planet orbiting the primary star.[19][20] An additional linear trend in the radial velocity data was noticed in 2006[21] that could have been due to another planet or to the stellar companion.[22] In 2012, additional measurements allowed the detection of a second planet. A third possible planet with a period of 108 days was seen in the data, but with a false alarm probability of five percent.[23] Another paper by the same team updated the parameters for b and c but did not mention the possible planet d.[24]

An astrometric measurement of HD 142 b's inclination and true mass was published in 2022 as part of Gaia DR3.[25] Another 2022 study determined the inclination and true mass of planet c, and confirmed the existence of planet d.[26]

The HD 142 A planetary system[25][26]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
d ≥0.260+0.032
−0.036 MJ 		0.474+0.021
−0.023 		108.5±0.1 0.130+0.103
−0.085 		— —
b 7.1±1.0 MJ 1.039+0.046
−0.051 		351.4±0.4 0.158+0.033
−0.030 		59±7° —
c 10.901+1.278
−0.937 MJ 		9.811+0.515
−0.520 		10,159.6+384.8
−321.9 		0.277+0.026
−0.027 		90.374+10.495
−12.319° 		—

See also

  • List of extrasolar planets

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. doi:10.1086/132034. Bibcode: 1987PASP...99..695R.  Vizier query form
  2. ↑ 2.0 2.1 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  3. ↑ 3.0 3.1 Olsen, E. H. (1994). "Stroemgren photometry of F- and G-type stars brighter than V = 9.6. I. UVBY photometry". Astronomy and Astrophysics Supplement Series 106: 257–266. Bibcode: 1994A&AS..106..257O.  Vizier catalog entry
  4. ↑ 4.0 4.1 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  5. ↑ 5.0 5.1 5.2 Eggleton, P. P.; Tokovinin, A.A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869–879. doi:10.1111/j.1365-2966.2008.13596.x. Bibcode: 2008MNRAS.389..869E. 
  6. ↑ 6.0 6.1 Gray, R. O. et al. (2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc - The Southern Sample". The Astronomical Journal 132 (1): 161–170. doi:10.1086/504637. Bibcode: 2006AJ....132..161G. 
  7. ↑ 7.0 7.1 Eggenberger, A. et al. (2007). "The impact of stellar duplicity on planet occurrence and properties I. Observational results of a VLT/NACO search for stellar companions to 130 nearby stars with and without planets". Astronomy and Astrophysics 474 (1): 273–291. doi:10.1051/0004-6361:20077447. Bibcode: 2007A&A...474..273E. http://www.aanda.org/articles/aa/full/2007/40/aa7447-07/aa7447-07.html. 
  8. ↑ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A. 
  9. ↑ 9.0 9.1 9.2 9.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  10. ↑ Holmberg (2009). "HD 142". Geneva-Copenhagen Survey of Solar neighbourhood III. http://vizier.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=V/130/gcs3&recno=18. 
  11. ↑ 11.0 11.1 11.2 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  12. ↑ 12.0 12.1 12.2 Ghezzi, L. et al. (September 2010), "Stellar Parameters and Metallicities of Stars Hosting Jovian and Neptunian Mass Planets: A Possible Dependence of Planetary Mass on Metallicity", The Astrophysical Journal 720 (2): 1290–1302, doi:10.1088/0004-637X/720/2/1290, Bibcode: 2010ApJ...720.1290G 
  13. ↑ 13.0 13.1 Soto, M. G.; Jenkins, J. S. (July 2018). "Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue". Astronomy & Astrophysics 615: 28. doi:10.1051/0004-6361/201731533. A76. Bibcode: 2018A&A...615A..76S. 
  14. ↑ 14.0 14.1 14.2 Tokovinin, A.; Kiyaeva, O. (February 2016). "Eccentricity distribution of wide binaries". Monthly Notices of the Royal Astronomical Society 456 (2): 2070–2079. doi:10.1093/mnras/stv2825. Bibcode: 2016MNRAS.456.2070T. 
  15. ↑ "HD 142". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+142. 
  16. ↑ "HD 142B". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+142B. 
  17. ↑ Valenti, J. A.; Fischer, D. A. (2005). "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs". The Astrophysical Journal Supplement Series 159 (1): 141–166. doi:10.1086/430500. Bibcode: 2005ApJS..159..141V. 
  18. ↑ Raghavan, Deepak et al. (2006). "Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems". The Astrophysical Journal 646 (1): 523–542. doi:10.1086/504823. Bibcode: 2006ApJ...646..523R. 
  19. ↑ "Astronomers close in on Solar System's 'siblings'" (Press release). Marsfield, New South Wales, Australia: Australian Astronomical Observatory. October 15, 2001. Archived from the original on August 22, 2016. Retrieved July 10, 2016.
  20. ↑ Tinney, C. G. et al. (2002). "Two Extrasolar Planets from the Anglo-Australian Planet Search". The Astrophysical Journal 571 (1): 528–531. doi:10.1086/339916. Bibcode: 2002ApJ...571..528T. 
  21. ↑ Butler, R. P. et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal 646 (1): 505–522. doi:10.1086/504701. Bibcode: 2006ApJ...646..505B. 
  22. ↑ Wright, J. T. et al. (2007). "Four New Exoplanets and Hints of Additional Substellar Companions to Exoplanet Host Stars". The Astrophysical Journal 657 (1): 533–545. doi:10.1086/510553. Bibcode: 2007ApJ...657..533W. 
  23. ↑ Wittenmyer, Robert A. et al. (2012). "The Anglo-Australian Planet Search. XXII. Two New Multi-planet Systems". The Astrophysical Journal 753 (2): 169. doi:10.1088/0004-637X/753/2/169. Bibcode: 2012ApJ...753..169W. 
  24. ↑ Wittenmyer, Robert A. et al. (2020). "Cool Jupiters greatly outnumber their toasty siblings: occurrence rates from the Anglo-Australian Planet Search". Monthly Notices of the Royal Astronomical Society 492 (1): 377–383. doi:10.1093/mnras/stz3436. Bibcode: 2020MNRAS.492..377W. 
  25. ↑ 25.0 25.1 Gaia Collaboration et al. (2023). "Gaia Data Release 3". Astronomy & Astrophysics 674: A34. doi:10.1051/0004-6361/202243782. 
  26. ↑ 26.0 26.1 Feng, Fabo et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series 262 (21): 21. doi:10.3847/1538-4365/ac7e57. Bibcode: 2022ApJS..262...21F. 

External links

Coordinates: Sky map 00h 06m 19.18s, −49° 04′ 30.7″



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