Jump to content

HD 43162

From Wikipedia, the free encyclopedia
(Redirected from HR 2225)

HD 43162
Location of HD 43162 (circled)
Observation data
Epoch J2000[1]      Equinox J2000[1]
Constellation Canis Major
HD 43162 A
Right ascension 06h 13m 45.29538s
Declination −23° 51′ 42.9715″
Apparent magnitude (V) +6.366[2]
HD 43162 B
Right ascension 06h 13m 45.40574s[3]
Declination −23° 52′ 07.5731″[3]
Apparent magnitude (V) +12.5 (combined)[4]
HD 43162 C
Right ascension 06h 13m 47.17685s[5]
Declination −23° 54′ 24.8191″[5]
Apparent magnitude (V) +12.96[6]
Characteristics
HD 43162 A
Spectral type G6.5V[6]
B−V color index 0.702[1]
J−H color index 0.266[1]
J−K color index 0.403[1]
Variable type BY Draconis variable
HD 43162 B
Spectral type M3.5 / M5[7]
J−H color index 0.579[3] / ?
J−K color index 0.835[3] / ?
HD 43162 C
Spectral type dM3.5e[8]
B−V color index 1.36[5]
J−H color index 0.563[5]
J−K color index 0.851[5]
Variable type Flare star
Astrometry
HD 43162 A
Radial velocity (Rv)21.91±0.09[1] km/s
Proper motion (μ) RA: -47.564[1] mas/yr
Dec.: 111.085[1] mas/yr
Parallax (π)59.885 ± 0.0192 mas[1]
Distance54.46 ± 0.02 ly
(16.699 ± 0.005 pc)
HD 43162 B
Radial velocity (Rv)22.9±0.2[3] km/s
Proper motion (μ) RA: -36.865[3] mas/yr
Dec.: 124.763[3] mas/yr
Parallax (π)59.377 ± 0.4216 mas[3]
Distance54.9 ± 0.4 ly
(16.8 ± 0.1 pc)
HD 43162 C
Proper motion (μ) RA: -31.239[5] mas/yr
Dec.: 111.054[5] mas/yr
Parallax (π)59.9905 ± 0.0222 mas[5]
Distance54.37 ± 0.02 ly
(16.669 ± 0.006 pc)
Orbit
PrimaryHD 43162 A
CompanionHD 43162 B
Semi-major axis (a)24[6]"
(410 AU[6])
Orbit
PrimaryHD 43162 A
CompanionHD 43162 C
Semi-major axis (a)164[6]"
(2740 AU[6])
Details[9]
HD 43162 A
Mass0.99±0.02 M☉
Surface gravity (log g)4.53±0.03 cgs
Temperature5661±27 K
Metallicity [Fe/H]0.057±0.022,[9] −0.02[10] dex
Rotation7.24±0.22 d[11]
Age1900±1300,[9] 295±36[11] Myr
HD 43162 Ba
Temperature3265+165
−85[7] K
HD 43162 Bb
Temperature3180+85
−170[7] K
Other designations
WDS J6138-2352AB
HD 43162 A: V352 CMa, CD−23° 3577, CPD−23° 1125, Gaia DR3 2913411183149615744, GC 7961, GJ 3389, HD 43162, HIP 29568, HR 2225, SAO 171428, PPM 250051, WDS J06138-2352A, TIC 124494439, TYC 6505-2273-1, GSC 06505-02273, 2MASS J06134528-2351433[1]
HD 43162 B: Gaia DR3 2913411183147100416, HD 43162B, WDS J06138-2352B, TIC 124494444, 2MASS J06134539-2352077, DENIS J061345.3-235207, WISE J061345.36-235206.3[3]
HD 43162 C: Gaia DR3 2913314288686472576, HD 43162C, WDS J06138-2352C, TIC 124494465, 2MASS J06134717-2354250, DENIS J061347.1-235424, WISE J061347.14-235423.7, WISEA J061347.14-235423.6, EUVE J0613-23.9B, USNO-B1.0 0660-00076188[5]
Database references
SIMBADA
B
C

HD 43162 is a star system consisting of a young solar analog star orbited by a pair of red dwarfs and another solitary red dwarf farther away. It is located about 54.5 light-years (16.7 parsecs) away in the southern constellation of Canis Major, making it one of the closest quadruple star systems. It has the variable star designation V352 Canis Majoris (often abbreviated to V352 CMa). With an apparent magnitude of 6.366, it is barely visible to the naked eye under dark skies far from city lights.

HD 43162 A

[edit]
Two light curves for HD 43162. The upper panel, plotted from TESS data,[12] shows the short term variability with the 7.2 day rotation period marked in red. The lower panel, adapted from Kajatkari et al.[11] shows the variability on a timescale of years, with yearly mean values plotted in purple.

HD 43162 A, often simply HD 43162, is an active G-type main sequence star with the spectral type G6.5V.[11] It is a BY Draconis variable[6] with a long brightness cycle lasting 11.7±0.5 years. Though estimates on the star's age vary substantially, the star is likely young based on the strong calcium H and K emission lines (wavelengths 3968.469 Å and 3933.663 Å[13]), high X-ray luminosity, rapid rotation, and its richness in lithium, though its metallicity ([Fe/H]) does not match the star's young age. The metallicity and its motion through space connotes that the star belongs to the young disk population,[11] part of the Milky Way's thin disk.[9]

The star has been noted to be abnormally poor in carbon, with a carbon-oxygen ratio calculated at [C/O]=−0.17±0.05 dex, despite having typical oxygen and iron abundances for solar-like stars. While oxygen is known to originate in the supernovae of massive stars, the origin of carbon remains unclear, and thus the reason for this anomalous carbon abundance is still unknown.[9]

In 2009, the star became one of eleven stars discovered to be surrounded by debris disks by the Spitzer Space Telescope, alongside planetary hosts such as Gliese 581, HD 40979, and HD 178911, the latter two also multiple star systems. No planets have been discovered around HD 43162 A, however, the only one out of the eleven without known exoplanets.[14]

Photometric data from the Hipparcos catalog indicates that the photometric variability of the star may be caused by an unresolved companion, which, if true, would make this component a binary system (Aa/Ab) itself,[6] which may push the number of stars in the whole system up to five.

HD 43162 Ba/Bb (2MASS J0613−2352 AB)

[edit]

HD 43162 B, also known as 2MASS J06134539−2352077, was announced to be a co-moving companion to HD 43162 A in 2013, located at a separation of 24 arcseconds (410 AU) from the primary star.[6] This object had been discovered to be a binary during the Astralux Large M-Dwarf Multiplicity Survey in 2012,[15] and the two components have been determined to be red dwarfs.

The larger of the pair (2MASS J0613−2352A) has a spectral type of M3.5 and a temperature of 3,265 K, while the smaller (B) has the spectral type M5.0 and a temperature of 3,180 K.[7] The two stars have a total mass of 0.57 M☉ or 0.42 M☉, with a mass ratio of 0.63:0.37. They orbit each other with a period of 13 years[16] at a distance of 3.91+0.83
−0.11 AU or 4.62+0.06
−0.04 AU, in a high eccentric orbit (eccentricity 0.77+0.10
−0.11 or 0.65±0.01). Due to the possible presence of missing mass, potential remains for the existence of another unseen body within the system.[17]

They are likely part of the Argus Association, which places their age at 45±5 Ma.[17]

HD 43162 C

[edit]

In 2010, the red dwarf 2MASS J06134717−2354250 was found to be a co-moving companion to HD 43162 A and was initially designated HD 43162 B,[18] before it was re-designated HD 43162 C in 2013.[6] It is situated 164 arcseconds away from the primary, which corresponds to a distance of 2,740 AU.[6] It is a coronally active flare star with a spectral type of dM3.5e.[4][19]

In 2003, before its physical association with the HD 43162 system was confirmed, the star was reported to have undergone a massive stellar flare, during which a 200-fold increase occurred in extreme ultraviolet (EUV) flux. This translates to a total energy of about 3×1034 ergs released in the 60–200 Å wavelength band, which is as energetic as the largest EUV flare that had been observed at the time,[8] seen on AU Microscopii in July 1992.[20]

See also

[edit]

References

[edit]
  1. ^ a b c d e f g h i "HD 43162". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 17 October 2024.
  2. ^ Høg, E.; et al. (February 2000). "The Tycho-2 Catalogue of the 2.5 Million Brightest Stars". Astronomy and Astrophysics. 355 (1): L27–L30. Bibcode:2000A&A...355L..27H.
  3. ^ a b c d e f g h i "HD 43162B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 17 October 2024.
  4. ^ a b Christian, D. J.; et al. (18 August 2003). "A New EUVE-detected Flare Star (EUVE J0613-23.9B)". Information Bulletin on Variable Stars. 5447 (1). Konkoly Observatory, Budapest: IAU. Bibcode:2003IBVS.5447....1C.
  5. ^ a b c d e f g h i "HD 43162C". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 17 October 2024.
  6. ^ a b c d e f g h i j k Chini, R.; et al. (8 November 2013). "New visual companions of solar-type stars within 25 pc". Monthly Notices of the Royal Astronomical Society. 437 (1). Oxford University Press (OUP): 879–886. arXiv:1310.2684. doi:10.1093/mnras/stt1953. ISSN 0035-8711.
  7. ^ a b c d Bergfors, C.; et al. (31 December 2015). "Characterization of close visual binaries from the AstraLux Large M Dwarf Survey". Monthly Notices of the Royal Astronomical Society. 456 (3). Oxford University Press (OUP): 2576–2585. arXiv:1511.09119. doi:10.1093/mnras/stv2768. ISSN 0035-8711.
  8. ^ a b Christian, D. J.; et al. (18 July 2003). "The Extreme-Ultraviolet Continuum of a Strong Stellar Flare". The Astrophysical Journal. 593 (2). American Astronomical Society: L105–L108. Bibcode:2003ApJ...593L.105C. doi:10.1086/378217. hdl:10211.3/172069. ISSN 0004-637X.
  9. ^ a b c d e Spina, Lorenzo; et al. (2016). "Planet signatures and effect of the chemical evolution of the Galactic thin-disk stars". Astronomy & Astrophysics. 585. EDP Sciences: A152. arXiv:1511.01012. Bibcode:2016A&A...585A.152S. doi:10.1051/0004-6361/201527429. ISSN 0004-6361.
  10. ^ Bodaghee, A.; et al. (2003). "Chemical abundances of planet-host stars". Astronomy & Astrophysics. 404 (2). EDP Sciences: 715–727. doi:10.1051/0004-6361:20030543. ISSN 0004-6361.
  11. ^ a b c d e Kajatkari, P.; et al. (2015). "Periodicity in some light curves of the solar analogue V352 Canis Majoris". Astronomy & Astrophysics. 577. EDP Sciences: A84. arXiv:1310.4280. Bibcode:2015A&A...577A..84K. doi:10.1051/0004-6361/201322847. ISSN 0004-6361.
  12. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  13. ^ Bjørgen, Johan P.; et al. (2018). "Three-dimensional modeling of the Ca II H and K lines in the solar atmosphere". Astronomy & Astrophysics. 611. EDP Sciences: A62. arXiv:1712.01045. Bibcode:2018A&A...611A..62B. doi:10.1051/0004-6361/201731926. ISSN 0004-6361.
  14. ^ Kóspál, Ágnes; Ardila, David R.; Moór, Attila; Ábrahám, Péter (10 July 2009). "On the Relationship Between Debris Disks and Planets". The Astrophysical Journal. 700 (2). American Astronomical Society: L73–L77. arXiv:0907.0028. Bibcode:2009ApJ...700L..73K. doi:10.1088/0004-637x/700/2/l73. ISSN 0004-637X.
  15. ^ Janson, Markus; et al. (3 July 2012). "The Astralux Large M-Dwarf Multiplicity Survey". The Astrophysical Journal. 754 (1). American Astronomical Society: 44. arXiv:1205.4718. Bibcode:2012ApJ...754...44J. doi:10.1088/0004-637x/754/1/44. ISSN 0004-637X.
  16. ^ Durkan, Stephen; et al. (2018). "A Radial velocity survey of spatially resolved young, low-mass binaries". Astronomy & Astrophysics. 618. EDP Sciences: A5. arXiv:1806.05133. Bibcode:2018A&A...618A...5D. doi:10.1051/0004-6361/201732156. ISSN 0004-6361.
  17. ^ a b Calissendorff, Per; et al. (29 September 2022). "Updated orbital monitoring and dynamical masses for nearby M-dwarf binaries". Astronomy & Astrophysics. 666. EDP Sciences: A16. arXiv:2208.09503. Bibcode:2022A&A...666A..16C. doi:10.1051/0004-6361/202142766. ISSN 0004-6361.
  18. ^ Raghavan, Deepak; et al. (13 August 2010). "A Survey of Stellar Families: Multiplicity of Solar-Type Stars". The Astrophysical Journal Supplement Series. 190 (1). American Astronomical Society: 1–42. arXiv:1007.0414. Bibcode:2010ApJS..190....1R. doi:10.1088/0067-0049/190/1/1. ISSN 0067-0049.
  19. ^ Kulkarni, Shrinivas R. (31 March 2005). The Nature of the Flaring EUVE Companion to HD 43162 (PDF) (Report). California Institute of Technology. Retrieved 18 October 2024.
  20. ^ Cully, Scott L.; et al. (1993). "Extreme Ultraviolet Explorer deep survey observations of a large flare on AU Microscopii". The Astrophysical Journal. 414. American Astronomical Society: L49. Bibcode:1993ApJ...414L..49C. doi:10.1086/186993. ISSN 0004-637X.
Retrieved from "https://en.wikipedia.org/w/index.php?title=HD_43162&oldid=1255790084"