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'''HD 43162''' is a multiple star system consisting of a young [[Solar analog]] star and three orbiting red dwarfs. It is located about {{convert|54.5|ly|pc|abbr=off}} away in the southern [[constellation]] of [[Canis Majoris]]. It has the [[variable star designation]] '''V352 Canis Majoris''' (sometimes 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''' is a star system consisting of a young [[Solar analog]] star and three orbiting red dwarfs. It is located about {{convert|54.5|ly|pc|abbr=off}} away in the southern [[constellation]] of [[Canis Majoris]], making it one of the closest quadruple star systems. It has the [[variable star designation]] '''V352 Canis Majoris''' (sometimes 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.
==Stellar components==
==Stellar components==
===HD 43162 A===
===HD 43162 A===
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[https://iopscience.iop.org/article/10.1086/378217/pdf Flare 2]
[https://iopscience.iop.org/article/10.1086/378217/pdf Flare 2]


==See also==
* [[HD 53680, HD 53705, and HD 53706]]: another quadruple system at a similar distance from Earth
==References==
==References==
{{reflist|refs=
{{reflist|refs=

Revision as of 02:27, 18 October 2024

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]
HD 43162 C
Right ascension 06h 13m 47.17685s[4]
Declination −23° 54′ 24.8191″[4]
Apparent magnitude (V) +12.96[5]
Characteristics
Spectral type G6.5V + (M3.5 + M5) + M4[5]
B−V color index 0.702[1] / ? / ? / 1.36[4]
J−H color index 0.266[1] / 0.579[3] / ? / 0.563[4]
J−K color index 0.403[1] / 0.835[3] / ? / 0.851[4]
Variable type BY Draconis variable (A)
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)
Orbit
PrimaryHD 43162 A
CompanionHD 43162 B
Semi-major axis (a)24[5]"
(410 AU[5])
Orbit
PrimaryHD 43162 A
CompanionHD 43162 C
Semi-major axis (a)164[5]"
(2740 AU[5])
Details[6]
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, −0.02[7] dex
Age1.9±1.3 Gyr
HD 43162 Ba
HD 43162 Bb
HD 43162 C
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[4]
Database references
SIMBADA
B
C

HD 43162 is a star system consisting of a young Solar analog star and three orbiting red dwarfs. It is located about 54.5 light-years (16.7 parsecs) away in the southern constellation of Canis Majoris, making it one of the closest quadruple star systems. It has the variable star designation V352 Canis Majoris (sometimes 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.

Stellar components

HD 43162 A

Anomalous carbon abundance Variability

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.[5]

HD 43162 B (2MASS J0613−2352 AB)

HD 43162 B, also known as 2MASS J06134539−2352077, was reported 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.[5] This object had been discovered to be a binary during the Astralux Large M-Dwarf Multiplicity Survey in 2012,[8] and the two components have been determined to be red dwarfs.

The larger component (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.[9] 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[10] at a distance of 3.91+0.83
−0.11 AU or 4.62+0.06
−0.04 AU, with a high eccentricity of 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.[11]

They are likely part of the Argus Association, which places their age at 45±5 Ma.[11]

HD 43162 C

In 2010, the M4-type red dwarf 2MASS J06134717−2354250 was found to be a co-moving companion to HD 43162 A and was initially designated HD 43162 B,[12] before it was re-designated HD 43162 C in 2013.[5] It is situated 164 arcseconds away from the primary, which corresponds to a distance of 2,740 AU.[5]

Flare Flare 2

See also

References

  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 c d e f "HD 43162C". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 17 October 2024.
  5. ^ a b c d e f g h i j Chini, R.; Fuhrmann, K.; Barr, A.; Pozo, F.; Westhues, C.; Hodapp, K. (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. doi:10.1093/mnras/stt1953. ISSN 0035-8711.
  6. ^ Spina, Lorenzo; Meléndez, Jorge; Ramírez, Ivan (2016). "Planet signatures and effect of the chemical evolution of the Galactic thin-disk stars". Astronomy & Astrophysics. 585. EDP Sciences: A152. doi:10.1051/0004-6361/201527429. ISSN 0004-6361.
  7. ^ Bodaghee, A.; Santos, N. C.; Israelian, G.; Mayor, M. (2003). "Chemical abundances of planet-host stars". Astronomy & Astrophysics. 404 (2). EDP Sciences: 715–727. doi:10.1051/0004-6361:20030543. ISSN 0004-6361.
  8. ^ Janson, Markus; Hormuth, Felix; Bergfors, Carolina; Brandner, Wolfgang; Hippler, Stefan; Daemgen, Sebastian; Kudryavtseva, Natalia; Schmalzl, Eva; Schnupp, Carolin; Henning, Thomas (3 July 2012). "The Astralux Large M-Dwarf Multiplicity Survey". The Astrophysical Journal. 754 (1). American Astronomical Society: 44. doi:10.1088/0004-637x/754/1/44. ISSN 0004-637X.
  9. ^ Bergfors, C.; Brandner, W.; Bonnefoy, M.; Schlieder, J.; Janson, M.; Henning, Th.; Chauvin, G. (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. doi:10.1093/mnras/stv2768. ISSN 0035-8711.
  10. ^ Durkan, Stephen; Janson, Markus; Ciceri, Simona; Brandner, Wolfgang; Schlieder, Joshua; Henning, Thomas; Bonnefoy, Mickaël; Kankare, Juliet; Watson, Christopher A. (2018). "A Radial velocity survey of spatially resolved young, low-mass binaries". Astronomy & Astrophysics. 618. EDP Sciences: A5. doi:10.1051/0004-6361/201732156. ISSN 0004-6361.
  11. ^ a b Calissendorff, Per; Janson, Markus; Rodet, Laetitia; Köhler, Rainer; Bonnefoy, Mickaël; Brandner, Wolfgang; Brown-Sevilla, Samantha; Chauvin, Gaël; Delorme, Philippe; Desidera, Silvano; Durkan, Stephen; Fontanive, Clemence; Gratton, Raffaele; Hagelberg, Janis; Henning, Thomas; Hippler, Stefan; Lagrange, Anne-Marie; Langlois, Maud; Lazzoni, Cecilia; Maire, Anne-Lise; Messina, Sergio; Meyer, Michael; Möller-Nilsson, Ole; Rabus, Markus; Schlieder, Joshua; Vigan, Arthur; Wahhaj, Zahed; Wildi, Francois; Zurlo, Alice (29 September 2022). "Updated orbital monitoring and dynamical masses for nearby M-dwarf binaries". Astronomy & Astrophysics. 666. EDP Sciences: A16. doi:10.1051/0004-6361/202142766. ISSN 0004-6361.
  12. ^ Raghavan, Deepak; McAlister, Harold A.; Henry, Todd J.; Latham, David W.; Marcy, Geoffrey W.; Mason, Brian D.; Gies, Douglas R.; White, Russel J.; ten Brummelaar, Theo A. (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. doi:10.1088/0067-0049/190/1/1. ISSN 0067-0049.
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