HD 142

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HD 142
Observation data
Epoch J2000.0       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  mas [9]
Distance 85.39 ± 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  mas [11]
Distance 85.31 ± 0.08  ly
(26.16 ± 0.02  pc)
Details [12]
HD 142 A
Mass 1.25±0.10  M☉
Radius 1.41±0.11  R☉
Luminosity 2.9  L☉
Surface gravity (log g)4.34±0.14  cgs
Temperature 6,338±46  K
Metallicity [Fe/H]0.03±0.04  dex
Rotational velocity (v sin i)9.58±0.74 [13]  km/s
Age 2.5  Gyr
HD 142 B
Mass 0.54 [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
SIMBAD data

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]

Contents

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  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±0.10.130+0.103
−0.085		——
b 7.1±1.0  MJ 1.039+0.046
−0.051		351.4±0.40.158+0.033
−0.030		59±7 ° —
c10.901+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

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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 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. 1 2 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. 1 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.
  5. 1 2 3 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. arXiv: 0806.2878 . Bibcode: 2008MNRAS.389..869E . doi: 10.1111/j.1365-2966.2008.13596.x .
  6. 1 2 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. arXiv: astro-ph/0603770 . Bibcode: 2006AJ....132..161G . doi: 10.1086/504637 .
  7. 1 2 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. Bibcode: 2007A&A...474..273E . doi: 10.1051/0004-6361:20077447 .
  8. ↑ 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.
  9. 1 2 3 4 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.
  10. ↑ Holmberg; et al. (2009). "HD 142". Geneva-Copenhagen Survey of Solar neighbourhood III. Retrieved 2010-01-27.
  11. 1 2 3 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.
  12. 1 2 3 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, arXiv: 1007.2681 , Bibcode: 2010ApJ...720.1290G , doi: 10.1088/0004-637X/720/2/1290
  13. 1 2 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. arXiv: 1801.09698 . Bibcode: 2018A&A...615A..76S . doi: 10.1051/0004-6361/201731533 . A76.
  14. 1 2 3 Tokovinin, A.; Kiyaeva, O. (February 2016). "Eccentricity distribution of wide binaries". Monthly Notices of the Royal Astronomical Society. 456 (2): 2070–2079. arXiv: 1512.00278 . Bibcode: 2016MNRAS.456.2070T . doi: 10.1093/mnras/stv2825 .
  15. ↑ "HD 142". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-08-12.
  16. ↑ "HD 142B". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-08-12.
  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. Bibcode: 2005ApJS..159..141V . doi: 10.1086/430500 .
  18. ↑ Raghavan, Deepak; et al. (2006). "Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems". The Astrophysical Journal. 646 (1): 523–542. arXiv: astro-ph/0603836 . Bibcode: 2006ApJ...646..523R . doi: 10.1086/504823 .
  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. arXiv: astro-ph/0111255 . Bibcode: 2002ApJ...571..528T . doi: 10.1086/339916 .
  21. ↑ Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv: astro-ph/0607493 . Bibcode: 2006ApJ...646..505B . doi: 10.1086/504701 .
  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. arXiv: astro-ph/0611658 . Bibcode: 2007ApJ...657..533W . doi: 10.1086/510553 .
  23. ↑ Wittenmyer, Robert A.; et al. (2012). "The Anglo-Australian Planet Search. XXII. Two New Multi-planet Systems". The Astrophysical Journal. 753 (2). 169. arXiv: 1205.2765 . Bibcode: 2012ApJ...753..169W . doi: 10.1088/0004-637X/753/2/169 .
  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. arXiv: 1912.01821 . Bibcode:2020MNRAS.492..377W. doi: 10.1093/mnras/stz3436 .
  25. 1 2 Gaia Collaboration; et al. (2023). "Gaia Data Release 3". Astronomy & Astrophysics. 674: A34. arXiv: 2206.05595 . Bibcode:2023A&A...674A..34G. doi:10.1051/0004-6361/202243782. S2CID   249626026.
  26. 1 2 Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series . 262 (21): 21. arXiv: 2208.12720 . Bibcode:2022ApJS..262...21F. doi: 10.3847/1538-4365/ac7e57 . S2CID   251864022.
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