wikilink variable star designation
|
Add: doi-access. | Use this bot. Report bugs. | Suggested by Headbomb | #UCB_toolbar
|
||
(6 intermediate revisions by 5 users not shown) | |||
Line 2: | Line 2: | ||
{{Starbox begin |
{{Starbox begin |
||
| name = AS Leonis Minoris |
| 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 |
{{Starbox observe |
||
Line 29: | Line 33: | ||
{{Starbox end}} |
{{Starbox end}} |
||
'''AS Leonis Minoris''' (AS LMi), also known as '''TYC 2505-672-1''', is an eclipsing binary system in the constellation of [[Leo Minor (constellation)|Leo Minor]]. It has by far the longest period, 69.1 years, of any known eclipsing binary.<ref name="Lipunov"/> During its roughly 3.45 year long eclipses, it fades by 4.5 magnitudes (about a factor of 60).<ref name="Rodriguez"/> |
'''AS Leonis Minoris''' (AS LMi), also known as '''TYC 2505-672-1''', is an [[eclipsing binary]] system in the constellation of [[Leo Minor (constellation)|Leo Minor]]. It has by far the longest period, 69.1 years, of any known eclipsing binary.<ref name="Lipunov"/> During its roughly 3.45 year long eclipses, it fades by 4.5 magnitudes (about a factor of 60).<ref name="Rodriguez"/> |
||
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/> |
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 |
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 (large [[Optical depth (astrophysics)|optical depth]]) disk.<ref name="Rodriguez"/> |
||
==References== |
==References== |
||
Line 42: | Line 46: | ||
<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=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 |doi=10.1051/0004-6361/201526528 |arxiv=1602.06010 |bibcode=2016A&A...588A..90L |s2cid=119116308 }}</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 |bibcode=2016AJ....151..123R |s2cid=24349954 |url=https://resolver.caltech.edu/CaltechAUTHORS:20160606-094933545 }}</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> |
<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> |
||
Line 61: | Line 65: | ||
{{DEFAULTSORT:AS Leonis Minoris}} |
{{DEFAULTSORT:AS Leonis Minoris}} |
||
[[Category:Algol variables]] |
[[Category:Algol variables]] |
||
[[Category:Leo Minor |
[[Category:Leo Minor]] |
||
[[Category:Objects with variable star designations|Leonis Minoris, AS]] |
[[Category:Objects with variable star designations|Leonis Minoris, AS]] |
| |
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Leo Minor |
Right ascension | 09h53m 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 as TYC 2505-672-1, is an eclipsing binary system in the constellation of Leo 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 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.[5] Because R Coronae Borealis variables fade repeatedly, the discovery of the star's dramatic brightness decline triggered a search of archival photographic plates for evidence of earlier dimming events.[6][7] Tang et al. used 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 ε 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 (large optical depth) disk.[4]