Gaia17bpp
{{short description|M-type star in the constellation Sagitta}}
{{Starbox begin
|name=Gaia17bpp
}}
{{Starbox image
|image=
|caption=An optical image of Gaia17bpp, captured by the Pan-STARRS1 telescope.
}}
{{Starbox observe
|constell=Sagitta{{cite constellation|Gaia17bpp}}
|epoch=J2000
|ra={{RA|19|37|23.16}}
|dec={{DEC|+17|59|02.9}}
}}
{{Starbox character
|type=Red giant branch{{cn|date=May 2025}}
|class=M0-III{{cn|date=May 2025}}
|j-k=1.7{{cn|date=May 2025}}
}}
{{Starbox astrometry
|parallax=−0.18
|p_error=0.4
|parallax_footnote={{efn|Derived distance using photogeometric distance posterior distribution (Bailer-Jones et al. 2021)}}
}}
{{Starbox detail
| mass = 1.5
| radius = 45
| temperature = 3,850
}}
{{Starbox catalog
|names=AT 2017exj, 2MASS J19372316+1759029, Gaia DR3 1824311891830344704
}}
{{Starbox reference
|Simbad=Gaia17bpp
}}
{{Starbox end}}
Gaia17bpp is a rare M-type red giant star that exhibited a single large dimming event (G-16-20.5 mag) over 6.5 years. It is located in the Sagitta constellation and is about 27,600 light years away from Earth.
Astronomical characteristics
The variable star is located in the constellation of Sagitta roughly 27,600 ly (8.5 kpc).{{Cite journal |last1=Tzanidakis |first1=Anastasios |last2=Davenport |first2=James R. A. |last3=Bellm |first3=Eric C. |last4=Wang |first4=Yuankun |date=2023-09-01 |title=Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event |journal=The Astrophysical Journal |volume=955 |issue=1 |pages=69 |doi=10.3847/1538-4357/aceda7 |doi-access=free |arxiv=2306.12409 |bibcode=2023ApJ...955...69T |issn=0004-637X}} Current hypothesis and archival data suggest that Gaia17bpp belongs to a rare family of ultra-long period binary stars where the companion is enshrouded in large optically thick disks reminiscent of Epsilon Aurigae, VVV-WIT-07, and AS Leonis Minoris.{{Cite journal |last1=Kloppenborg |first1=Brian |last2=Stencel |first2=Robert |last3=Monnier |first3=John D. |last4=Schaefer |first4=Gail |last5=Zhao |first5=Ming |last6=Baron |first6=Fabien |last7=McAlister |first7=Hal |last8=ten Brummelaar |first8=Theo |last9=Che |first9=Xiao |last10=Farrington |first10=Chris |last11=Pedretti |first11=Ettore |last12=Sallave-Goldfinger |first12=P. J. |last13=Sturmann |first13=Judit |last14=Sturmann |first14=Laszlo |last15=Thureau |first15=Nathalie |date=2010-04-01 |title=Infrared images of the transiting disk in the ɛ Aurigae system |url=https://ui.adsabs.harvard.edu/abs/2010Natur.464..870K |journal=Nature |volume=464 |issue=7290 |pages=870–872 |doi=10.1038/nature08968 |pmid=20376144 |arxiv=1004.2464 |bibcode=2010Natur.464..870K |s2cid=18866716 |issn=0028-0836}}{{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. |date=2016-04-01 |title=Discovery of an unusual bright eclipsing binary with the longest known period: TYC 2505-672-1/MASTER OT J095310.04+335352.8 |url=https://ui.adsabs.harvard.edu/abs/2016A&A...588A..90L |journal=Astronomy and Astrophysics |volume=588 |pages=A90 |doi=10.1051/0004-6361/201526528 |arxiv=1602.06010 |bibcode=2016A&A...588A..90L |issn=0004-6361}}{{Cite journal |last1=Smith |first1=Leigh C. |last2=Koposov |first2=Sergey E. |last3=Lucas |first3=Philip W. |last4=Sanders |first4=Jason L. |last5=Minniti |first5=Dante |last6=Udalski |first6=Andrzej |last7=Evans |first7=N. Wyn |last8=Aguado |first8=David |last9=Ivanov |first9=Valentin D. |last10=Saito |first10=Roberto K. |last11=Fraga |first11=Luciano |last12=Pietrukowicz |first12=Pawel |last13=Penoyre |first13=Zephyr |last14=González-Fernández |first14=Carlos |date=2021-08-01 |title=VVV-WIT-08: the giant star that blinked |journal=Monthly Notices of the Royal Astronomical Society |volume=505 |issue=2 |pages=1992–2008 |doi=10.1093/mnras/stab1211 |doi-access=free |arxiv=2106.05300 |bibcode=2021MNRAS.505.1992S |issn=0035-8711}} The proposed secondary star and disk remain unconfirmed due to the copious amount of intervening interstellar dust, and likely due to the remarkable long timescale period of the system.
Discovery and dimming event
File:Gaia17bppLightCurve.png for Gaia17bpp, showing the recovery from the dimming event. Adapted from Tzanidakis et al.]]
Gaia17bpp{{Cite web |title=Gaia17bpp |url=https://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia17bpp/ |access-date=2024-01-08 |website=gsaweb.ast.cam.ac.uk}} was initially discovered through the ESA's Gaia Photometric Science Alerts{{Cite journal |last1=Hodgkin |first1=S. T. |last2=Harrison |first2=D. L. |last3=Breedt |first3=E. |last4=Wevers |first4=T. |last5=Rixon |first5=G. |last6=Delgado |first6=A. |last7=Yoldas |first7=A. |last8=Kostrzewa-Rutkowska |first8=Z. |last9=Wyrzykowski |first9=Ł. |last10=van Leeuwen |first10=M. |last11=Blagorodnova |first11=N. |last12=Campbell |first12=H. |last13=Eappachen |first13=D. |last14=Fraser |first14=M. |last15=Ihanec |first15=N. |date=2021-08-01 |title=Gaia Early Data Release 3. Gaia photometric science alerts |url=https://ui.adsabs.harvard.edu/abs/2021A&A...652A..76H |journal=Astronomy and Astrophysics |volume=652 |pages=A76 |doi=10.1051/0004-6361/202140735 |arxiv=2106.01394 |bibcode=2021A&A...652A..76H |issn=0004-6361}} (GPSA) in 2022 by astronomers at the University of Washington.{{Cite web |last=Strickland |first=Ashley |date=2023-01-11 |title=Unusually brightening star captures attention as a stellar oddity |url=https://www.cnn.com/2023/01/11/world/distant-star-brightening-scn/index.html |access-date=2024-01-08 |website=CNN |language=en}}{{Cite web |title=The seven-year photobomb: Distant star's dimming was likely a 'dusty' companion getting in the way, astronomers say |url=https://www.washington.edu/news/2023/01/10/dusty-binary/ |access-date=2024-01-08 |website=UW News |language=en}} The remarkable Gaia17bpp dimming event occurred in mid 2012, however the GPSA issued an alert back in 2017 when the star began re-brightening. Due to the large duration of the dimming event, the entirety of the Gaia17bpp dimming event was recovered from several public data archives such as Pan-STARRS, and NASA's Wide-field Infrared Survey Explorer (WISE) where the dimming event was also observed in the near-infrared.
Researchers employed archival image searching and conducted spectroscopic follow-up observations on Gaia17bpp using the Apache Point Observatory 3.5m ARC Telescope.{{Cite web |title=ARC |url=https://arc.apo.nmsu.edu/ |access-date=2024-01-08 |website=arc.apo.nmsu.edu}} Throughout their analysis, they successfully ruled out several suspected variable star classes with similar dimming event such as R Coronae Borealis, Cataclysmic variable star, or Young stellar object.
Modeling of the dimming event suggest that a possible scenario includes the occultation of an extended oblate optically thick disk with 1.4 AU radius, moving with a transverse velocity of approximately 0.005 km/s. It is unclear how such large optically thick disks can form such in the case of Gaia17bpp and other analog systems. One study suggests that previous mass-transfer interaction between a close binary can produce large disks and lose angular momentum to produce the observed long period binary system.{{Cite web |last=Gibson |first=Justus |date=13 March 2018 |title=MESA models of the evolutionary state of the interacting binary epsilon Aurigae |url=https://academic.oup.com/mnras/article/476/4/5026/4931777 |access-date=2024-01-08 |website=academic.oup.com}}
See also
Notes
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