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wl eclipsing binary
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{{Starbox begin
| name = AS Leonis Minoris
}}
{{Starbox image
| image = [[Image:ASLMiLightCurve.png|250px]]
| caption = 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 Lipunov ''et al.'' (2016)<ref name="Lipunov"/>
}}
{{Starbox observe
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AS LMi's variability was first detected in 2013, during a search for "disappearing stars" in the [[MASTER]] database. It was initially thought to be an [[R Coronae Borealis variable]] star, although its fading was unusually slow for an R Coronae Borealis variable.<ref name="AT4784"/> Because R Coronae Borealis variables fade repeatedly, the discovery of the star's dramatic brightness decline triggered a search of archival [[Photographic_plate#Astronomy|photographic plates]] for evidence of earlier dimming events.<ref name=AT4787/><ref name=AT4788/> Tang ''et al.'' used [[Digital_Access_to_a_Sky_Century_@_Harvard|DASCH]] 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 the [[epsilon aurigae|ε Aurigae]] system.<ref name=Tang/>
The binary system
==References==
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<ref name=ivsi>{{cite web |title=AS LMi |url=https://www.aavso.org/vsx/index.php?view=detail.top&oid=297394 |website=The International Variable Star Index |publisher=AAVSO |access-date=7 December 2021}}</ref>
<ref name="Lipunov">{{cite journal |last1=Lipunov |first1=V. |last2=Gorbovskoy |first2=E. |last3=Afanasiev |first3=V. |last4=Tatarnikova |first4=A. |last5=Denisenko |first5=D. |last6=Makarov |first6=D. |last7=Tiurina |first7=N. |last8=Krushinsky |first8=V. |last9=Vinokurov |first9=A. |last10=Balanutsa |first10=P. |last11=Kuznetsov |first11=A. |last12=Gress |first12=O. |last13=Sergienko |first13=Yu. |last14=Yurkov |first14=V. |last15=Gabovich |first15=A. |last16=Tlatov |first16=A. |last17=Senik |first17=V. |last18=Vladimirov |first18=V. |last19=Popova |first19=E. |title=Discovery of an unusual bright eclipsing binary with the longest known period: TYC 2505-672-1/MASTEROTJ095310.04+335352.8 |journal=Astronomy & Astrophysics |date=April 2016 |volume=588 |pages=A90 |doi=10.1051/0004-6361/201526528 |arxiv=1602.06010 |bibcode=2016A&A...588A..90L |s2cid=119116308 }}</ref>
<ref name="Rodriguez">{{cite journal |last1=Rodriguez |first1=Joseph E. |last2=Stassun |first2=Keivan G. |last3=Lund |first3=Michael B. |last4=Siverd |first4=Robert J. |last5=Pepper |first5=Joshua |last6=Tang |first6=Sumin |last7=Kafka |first7=Stella |last8=Gaudi |first8=B. Scott |last9=Conroy |first9=Kyle E. |last10=Beatty |first10=Thomas G. |last11=Stevens |first11=Daniel J. |last12=Shappee |first12=Benjamin J. |last13=Kochanek |first13=Christopher S. |title=An Extreme Analogue of ɛ Aurigae: An M-giant Eclipsed Every 69 Years by a Large Opaque Disk Surrounding a Small Hot Source |journal=The Astronomical Journal |date=May 2016 |volume=151 |issue=5 |page=123 |doi=10.3847/0004-6256/151/5/123 |arxiv=1601.00135 |bibcode=2016AJ....151..123R |s2cid=24349954 |url=https://resolver.caltech.edu/CaltechAUTHORS:20160606-094933545 |doi-access=free }}</ref>
<ref name="AT4784">{{cite journal |last1=Denisenko |first1=D.|display-authors=etal |title=Optical "anti-transient" detected by MASTER |journal=The Astronomer's Telegram |date=4 February 2013 |volume=4784 |page=1|bibcode=2013ATel.4784....1D }}</ref>
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{{DEFAULTSORT:AS Leonis Minoris}}
[[Category:Algol variables]]
[[Category:Leo Minor
[[Category:Objects with variable star designations|Leonis Minoris, AS]]
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