# HD 43162

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

## HD 43162 A

HD 43162 A, often simply HD 43162, is an active G-type main sequence star with the spectral type G6.5V. It is a BY Draconis variable 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), 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, part of the Milky Way's thin disk.
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.
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.
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, 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. This object had been discovered to be a binary during the Astralux Large M-Dwarf Multiplicity Survey in 2012, 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. 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 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.
They are likely part of the Argus Association, which places their age at 45±5 Ma.

## 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, before it was re-designated HD 43162 C in 2013. It is situated 164 arcseconds away from the primary, which corresponds to a distance of 2,740 AU. It is a coronally active flare star with a spectral type of dM3.5e.
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 3×10$^{34}$ 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, seen on AU Microscopii in July 1992.