HD 43162

Last updated

HD 43162
Canis Major constellation map.svg
Red circle.svg
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]
Distance 54.46 ± 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]
Distance 54.9 ± 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]
Distance 54.37 ± 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
Mass 0.99±0.02  M☉
Surface gravity (log g)4.53±0.03  cgs
Temperature 5661±27  K
Metallicity [Fe/H]0.057±0.022, [9] −0.02 [10]   dex
Rotation 7.24±0.22  d [11]
Age 1900±1300, [9] 295±36 [11]   Myr
HD 43162 Ba
Temperature 3265+165
−85 [7]   K
HD 43162 Bb
Temperature 3180+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
SIMBAD A
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. With an apparent magnitude of 6.366, it is barely visible to the naked eye under dark skies far from city lights.

Contents

In 1999, Giuseppe Cutispoto et al. announced their discovery that HD 43162 is a variable star. [12] It was given its variable star designation, V352 Canis Majoris (often abbreviated to V352 CMa), in 2006. [13]

HD 43162 A

Two light curves for HD 43162. The upper panel, plotted from TESS data, shows the short term variability with the 7.2 day rotation period marked in red. The lower panel, adapted from Kajatkari et al. shows the variability on a timescale of years, with yearly mean values plotted in purple. V352CMaLightCurve.png
Two light curves for HD 43162. The upper panel, plotted from TESS data, shows the short term variability with the 7.2 day rotation period marked in red. The lower panel, adapted from Kajatkari et al. 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 [15] ), 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. [16]

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)

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, [17] 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 [18] 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. [19]

They are likely part of the Argus Association, which places their age at 45±5  Ma . [19]

HD 43162 C

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, [20] 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] [21]

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. [22]

See also

Related Research Articles

<span class="mw-page-title-main">70 Ophiuchi</span> Star in the constellation Ophiuchus

70 Ophiuchi is a binary star system located 16.6 light years away from the Earth. It is in the constellation Ophiuchus. At magnitude 4 it appears as a dim star visible to the unaided eye away from city lights.

Struve 2398 is a binary star system in the northern constellation of Draco. Struve 2398 is star number 2398 in the Struve Double Star Catalog of Russian-German astronomer Friedrich Georg Wilhelm von Struve. The astronomer's surname, and hence the star identifier, is sometimes indicated by a Greek sigma, Σ; hence, this system can be listed with the identifier Σ 2398. Although the components are too faint to be viewed with the naked eye, this star system is among the closest to the Sun. Parallax measurements by the Gaia spacecraft give them an estimated distance of 11.5 light-years away.

<span class="mw-page-title-main">AD Leonis</span> M-type star in the constellation Leo

AD Leonis (Gliese 388) is a red dwarf star. It is located relatively near the Sun, at a distance of 16.2 light-years, in the constellation Leo. AD Leonis is a main sequence star with a spectral classification of M3.5V. It is a flare star that undergoes random increases in luminosity.

<span class="mw-page-title-main">Alpha Caeli</span> Brightest star in the constellation Caelum

Alpha Caeli is the brightest star in the constellation Caelum. It is in fact a binary star, made up of a F-type star of magnitude 4.46 and a red dwarf of magnitude 12.5. They are separated by 6.6" in the sky. Parallax measurements by the Gaia spacecraft imply a distance of 20.4 pc (67 ly) to Alpha Caeli. A debris disk has been detected around the primary component of the system.

<span class="mw-page-title-main">AB Doradus</span> Pre-main sequence star system in the constellation Dorado

AB Doradus is a pre-main-sequence quadruple star system in the constellation Dorado. The primary is a flare star that shows periodic increases in activity.

<span class="mw-page-title-main">GJ 1245</span> Triple star system in the constellation Cygnus

GJ 1245 is a double star with components G 208-44 and G 208-45, located 15.2 light-years away in the constellation Cygnus. G 208-44 is itself a closer double star made up of two red dwarfs, while G 208-45 is also a red dwarf. GJ 1245 is the 43rd closest stellar system to the Solar System. GJ 1245 A and B are active flare stars, and the pair are collectively designated V1581 Cygni.

<span class="mw-page-title-main">Ross 458</span> Star in the constellation Virgo

Ross 458, also referred to as DT Virginis, is a binary star system in the constellation of Virgo. It has an apparent visual magnitude of 9.79 and is located at a distance of 37.6 light-years from the Sun. Both of the stars are low-mass red dwarfs with at least one of them being a flare star. This binary system has a circumbinary sub-stellar companion.

<span class="mw-page-title-main">V538 Aurigae</span> Star in constellation Auriga

V538 Aurigae is a single star in the northern constellation of Auriga. With an apparent visual magnitude of 6.23, this star requires good dark sky conditions to view with the naked eye. It is located at a distance of 40.0 light-years (12.3 pc) from Sun based on parallax. The star is drifting further away with a radial velocity of 0.9 km/s. It is a member of the Local Association, and is most likely a thin disk star.

GJ 3379 is the nearest star in the Orion constellation, located at a distance of 17 light years from the Sun based on parallax. It is a single star with an apparent visual magnitude of +11.31 and an absolute magnitude of +12.71, therefore, the star is not visible with the naked eye. It is positioned in the upper left part of the Orion constellation, to the SSE of Betelgeuse. This star is drifting further away with a radial velocity of +30.0 kilometers per second. In the past, this star had a relatively close encounter with the Solar System. Some 161,000±6,000 years ago, it achieved a minimum distance of 4.08 ± 0.20 ly (1.25 ± 0.06 pc).

<span class="mw-page-title-main">Gliese 752</span> Binary star system in the constellation Aquila

Gliese 752 is a binary star system in the Aquila constellation. This system is relatively nearby, at a distance of 19.3 light-years.

<span class="mw-page-title-main">YZ Canis Minoris</span> Star in the constellation Canis Minor

YZ Canis Minoris is a red-hued star in the equatorial constellation of Canis Minor. With an apparent visual magnitude of 11.15, it is much too faint to be viewed with the naked eye. The distance to YZ CMi can be estimated from its annual parallax shift of 167 mas, yielding a value of 19.5 light years. Presently the star is moving further away with a heliocentric radial velocity of +26.5 km/s. It made its closest approach some 162,000 years ago when it made perihelion passage at a distance of 10.2 ly. YZ CMi is a potential member of the Beta Pictoris moving group.

ο Gruis, Latinised as Omicron Gruis, is a binary or triple star system in the southern constellation of Grus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.52. Based upon an annual parallax shift of 32.50 mas as seen from the Earth, the system is located 100 light years from the Sun.

<span class="mw-page-title-main">HN Pegasi</span> Star in the constellation Pegasus

HN Pegasi is the variable star designation for a young, Sun-like star in the northern constellation of Pegasus. It has an apparent visual magnitude of 5.9, which, according to the Bortle scale, indicates that it is visible to the naked eye from suburban skies. Parallax measurements put the star at a distance of around 59 light years from the Sun, but it is drifting closer with a radial velocity of −16.7 km/s.

<span class="mw-page-title-main">Gliese 569</span> Nearby red dwarf in the constellation Boötes

Gliese 569 is a ternary star system composed of a main-sequence star orbited by a pair of brown dwarfs in the constellation of Boötes about 32 light years away.

<span class="mw-page-title-main">V773 Tauri</span> Star system in the constellation Taurus

V773 Tauri is a young, multiple star system in the central region of Taurus, an equatorial constellation. This is a T Tauri-type variable star that ranges in apparent visual magnitude from 10.59 down to 10.95, which is too faint to be viewed with the naked eye. Based on various estimates, the system is located at a distance of approximately 433 light years from the Sun. It lies near the dark cloud Lynds 1495.

References

  1. 1 2 3 4 5 6 7 8 9 10 "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. 1 2 3 4 5 6 7 8 9 "HD 43162B". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 17 October 2024.
  4. 1 2 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. 1 2 3 4 5 6 7 8 9 "HD 43162C". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 17 October 2024.
  6. 1 2 3 4 5 6 7 8 9 10 11 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. 1 2 3 4 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. 1 2 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. 1 2 3 4 5 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. 1 2 3 4 5 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. ↑ Cutispoto, G.; Pastori, L.; Tagliaferri, G.; Messina, S.; Pallavicini, R. (July 1999). "Classification of EUV stellar sources detected by the ROSAT WFC. I. Photometric and radial velocity studies" (PDF). Astronomy and Astrophysics Supplement. 138: 87–99. doi:10.1051/aas:1999497 . Retrieved 3 January 2025.
  13. ↑ Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (August 2006). "The 78th Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 5721. Bibcode:2006IBVS.5721....1K . Retrieved 3 January 2025.
  14. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  15. ↑ 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.
  16. ↑ 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.
  17. ↑ 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.
  18. ↑ 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.
  19. 1 2 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.
  20. ↑ 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.
  21. ↑ 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.
  22. ↑ 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.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.