  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Puppis |
| Right ascension | 07h 13m 32.31810s [1] |
| Declination | −44° 38′ 23.0630″ [1] |
| Apparent magnitude (V) | 5.10 [2] 2.6–6 (GCVS) [3] 6–8 (1995 – ) [4] |
| Characteristics | |
| Spectral type | M5IIIe [3] |
| U−B color index | +1.24 [2] |
| B−V color index | +1.56 [2] |
| Variable type | SRb [3] |
| Astrometry | |
| Radial velocity (Rv) | 33.0 [5] km/s |
| Proper motion (μ) | RA: 106.31 [1] mas/yr Dec.: 324.99 [1] mas/yr |
| Parallax (π) | 15.61 ± 0.99 mas [1] |
| Distance | 210 ± 10 ly (64 ± 4 pc) |
| Details | |
| Mass | 0.659±0.043 [5] M☉ |
| Radius | 123±14 [5] R☉ |
| Luminosity | 2,000±17 [5] L☉ |
| Surface gravity (log g) | 0.078±0.027 [5] cgs |
| Temperature | 3,500±250 [5] K |
| Age | 10 [5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
(Credit: ESO/P. Kervella)
L2 Puppis (also known as HD 56096) is a giant star in the constellation of Puppis and is located between the bright stars Canopus and Sirius. It is a semi-regular pulsating star.
The designation L2 has a tangled history. This star and another were both labelled with "L" by Nicolas-Louis de Lacaille when he created the constellation Puppis within Argo Navis. [6] The two stars were labelled as "1.L" and "2.L" by Johann Elert Bode in his star catalogue published in 1801. [7] Later authors used L1 and L2, usually with numeric subscripts (i.e. L1 and L2), [8] but occasionally as superscripts. [9] The subscripted designation is now universally used where typography allows for subscripts. [5] [10]
L2 Puppis was discovered to be variable by Benjamin Apthorp Gould in 1872, [11] and was listed in Uranometria Argentina as 73 G. Puppis with magnitude 5.10v. It has never been given a formal variable star designation, unlike L1 Puppis which is OU Puppis. [12]
L2 Puppis varies in apparent magnitude by about two magnitudes with a period of 140 days. The average brightness also varies slowly over several years so that the total range is given as magnitude 2.6–6.0. Since 1995 the average brightness has dropped so that the 140-day variations are now between about magnitude 6 and 8. [4] [14] The variation in light may be caused by a combination of radial pulsations in the star's atmosphere and by dimming from circumstellar dust. [15]
L2 Puppis is most likely an asymptotic giant branch star that has passed through the main sequence and is evolving to become a white dwarf. It is shedding mass at the rate of about 5×10−7 M☉ per year, forming a circumstellar dust disk and bipolar plumes of gas that are thought to be the start of a "butterfly"-type planetary nebula. [5]
It has been calculated that the mass of L2 Puppis is currently about 0.66 M☉ and its original mass was close to one M☉ about 10 billion years ago. [5] Other calculations give higher masses, for example 2+1
−0.5 M☉, and younger ages such as 1.5 billion years. [10]
A candidate exoplanet has been found orbiting L2 Puppis every 4.69 years at a distance of 2.43 AU . The mass is highly uncertain, at 12 ± 16 MJ, and it might just be a dense clump of gas and dust. [5]
L2 Puppis has a visual 12th-magnitude companion. A hundred years ago, they were separated by about a minute of arc, but different proper motions mean that this is now about 1.5′ . [16]
