 A light curve for AS Leonis Minoris. The main plot shows the full light curve, and the inset shows the time around minimum brightness at an expanded scale. Adapted from Lipunovet al. (2016)[1] | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Leo Minor |
| Right ascension | 09h 53m 10.001s[2] |
| Declination | +33° 53′ 52.76″[2] |
| Apparent magnitude (V) | 10.7 - 15.4[3] |
| Characteristics | |
| Variable type | Algol[3] |
| Astrometry | |
| Radial velocity (Rv) | -56.14[2] km/s |
| Proper motion (μ) | RA: 3.054±0.077[2]mas/yr Dec.: −11.645±0.071[2]mas/yr |
| Parallax (π) | 0.6994±0.0513 mas[2] |
| Distance | 4,700 ± 300 ly (1,400 ± 100 pc) |
| Other designations | |
| AS LMi,TYC 2505-672-1,MASTER OT J095310.04+335352.8,IRAS F09501+3408,2MASS J09531000+3353527 | |
| Database references | |
| SIMBAD | data |
AS Leonis Minoris (AS LMi), also known asTYC 2505-672-1, is aneclipsing binary system in the constellation ofLeo Minor. It has by far the longest period, 69.1 years, of any known eclipsing binary.[1] During its roughly 3.45 year long eclipses, it fades by 4.5 magnitudes (about a factor of 60).[4]
AS LMi's variability was first detected in 2013, during a search for "disappearing stars" in theMASTER database. It was initially thought to be anR Coronae Borealis variable star, although its fading was unusually slow for an R Coronae Borealis variable.[5] Because R Coronae Borealis variables fade repeatedly, the discovery of the star's dramatic brightness decline triggered a search of archivalphotographic plates for evidence of earlier dimming events.[6][7] Tanget al. usedDASCH to search the large collection of Harvard photographic plates, and found that the star had dimmed for three years during the 1940s. They recognized that AS LMi is a very long period eclipsing binary, similar to theε Aurigae system.[8]
The binary system consists of an M-giant primary star orbited by a small hot secondary star that is itself surrounded by an optically thick (largeoptical depth) disk.[4]
