List of stars that have unusual dimming periods

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Artist's concept of an "uneven ring of dust" orbiting KIC 8462852, also known as Tabby's Star PIA22081-KIC8462852-TabbysStar-UnevenDustRing-Illustration-20171004.png
Artist's concept of an "uneven ring of dust" orbiting KIC 8462852, also known as Tabby's Star

This list of stars that have unusual dimming periods is a table of stars that have been observed to darken and brighten and do not appear to be eclipsing binaries or intrinsic variables. It is based on studies searching for analogs of Tabby's Star. [1] [2]

Contents

The listing here is ordered alphabetically.

List

Tabby's Star (KIC 8462852) - Consolidated plot of all known dimmings (1 March 2020) Consolidated plot of KIC 8462852 dip maxima March 2020 update.png
Tabby's Star (KIC 8462852) – Consolidated plot of all known dimmings (1 March 2020)
Star designation Stellar
class 		Magnitude Right ascension
(J2000)		 Declination
(J2000)		 Distance
(light-years)		Reason for dimming
Apparent Absolute
ASASSN-V J193622.23+115244.1 —14.0–15.5 [3] —19h 36m 22.23s [3] +11° 52′ 44.1″ [3] 6592 [3] Unknown
ASASSN-V J213939.3-702817.4 F0V [4] 12.95–14.22 [5] 2.5 [5] 21h 39m 39.3s [5] −70° 28′ 17.4″ [5] 3630 [4] Unknown
Betelgeuse M1-2 [6] +0.50 [7] —05h 55m 10.30536s [8] +07° 24′ 25.4304″ [8] —"large-grain circumstellar dust" [9] [10]
EPIC 204278916 M1 [11] 13.7 [12] —16h 02m 07.576s [13] −22° 57′ 46.89″ [13] — Dust disk
EPIC 204376071 M [14] ——16h 04m 10.1267s [15] −22° 34′ 45.5503″ [15] 440 [14] Possibly giant planet or brown dwarf with rings
HD 139139
(EPIC 249706694)		G3/5V9.84; [16] 9.677 [17] —15h 37m 06.215s [17] −19° 08′ 32.96″ [17] 350 [18]
572 [17] 		Unknown
KH 15D K7 [19] 15.5–21.5 [20] 6.226 [21] 06h 41m 10.31s [22] +09° 28′ 33.2″ [22] 773 [23] Possibly circumbinary disk
KIC 4150611
(HD 181469)		Pulsator/K/M/G——19h 18m 58.21759s [24] +39° 16′ 01.7913″ [24] —Five-star system
PDS 110 keF6 IVeb [25] 10.422 [25] 2.54 [25] 05h 23m 31.008s [25] –01° 04′ 23.68″ [25] 1090 [25] Possibly giant planet or brown dwarf with disc of dust or large ring system
RW Cephei K2 0-Ia [26] 6.0–7.6 [27] —22h 23m 07.01521s [28] +55° 57′ 47.6244″ [28] 11,000 [29] [lower-alpha 1] Unknown
RZ Piscium K0 IV [30] 11.29–13.82 [30] —01h 09m 42.056s [31] +27° 57′ 1.95″ [31] 550 [32] Substantial mass of gas and dust, possibly from disrupted planet
Tabby's Star
(KIC 8462852)		F3V [33] [34] 11.705 [34] 3.08 [33] 20h 06m 15.4527s [33] +44° 27′ 24.791″ [33] 1470 [33] Unknown
TIC 400799224——————"probably from an orbiting body that periodically emits clouds of dust that occult the star" [35] [36]
V1400 Centauri K5 IV(e) Li [37] 12.31 [37] —14h 07m 47.93s [37] −39° 45′ 42.7″ [37] 434 [38] Planet with gigantic ring system
VVV-WIT-07 —14.35–16.164 [39] —17h 26m 29.387s [39] −35° 40′ 6.20″ [39] 23000/? [39] Unknown
WD 1145+017
(EPIC 201563164)		DB [40] 17.0 [41] —11h 48m 33.63s [40] +01° 28′ 59.4″ [40] 570 [42] Dust disk
ZTF J0139+5245
(ZTF J013906.17+524536.89)		DA [43] 18.4 [43] —01h 39m 06.17s+52° 45′ 36.89″564 [43] Dust disk

See also

Notes

  1. ↑ Assuming membership to Cepheus OB1

Related Research Articles

<span class="mw-page-title-main">Groombridge 34</span> Binary star system in the constellation of Andromeda

Groombridge 34 is a binary star system in the northern constellation of Andromeda. It was listed as entry number 34 in A Catalogue of Circumpolar Stars, published posthumously in 1838 by British astronomer Stephen Groombridge. Based upon parallax measurements taken by the Gaia spacecraft, the system is located about 11.6 light-years from the Sun. This positions the pair among the nearest stars to the Solar System.

36 Arietis is a star in the northern constellation of Aries. 36 Arietis is the Flamsteed designation. It is a dim, orange-hued star that is a challenge to view with the naked eye, having an apparent visual magnitude of 6.40. Based upon an annual parallax shift of 8.59±0.04 mas, this star is located 380 light-years away from the Sun. It is moving closer to the Earth with a heliocentric radial velocity of −34 km/s, and is a member of the Wolf 630 moving group of stars that share a common motion through space.

<span class="mw-page-title-main">21 Aquilae</span> Star in the constellation Aquila

21 Aquilae is a solitary variable star in the equatorial constellation of Aquila. It has the variable star designation V1288 Aql; 21 Aquilae is its Flamsteed designation. This object is visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of about 5.1. The star is located at a distance of around 680 light-years from Earth, give or take a 20 light-year margin of error. It is moving closer to the Earth with a heliocentric radial velocity of –5 km/s.

HD 142 is a wide binary star system in the southern constellation of Phoenix. The main component has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.7. The system is located at a distance of 85.5 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of +6 km/s.

HD 89744 is a star in the northern circumpolar constellation of Ursa Major, positioned about 0.4° due south of the bright star Tania Australis. This object has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.73. The distance to this star has been measured using the parallax method, which locates it 126 light years from the Sun. It is drifting closer with a radial velocity of −4.4 km/s. There are two known exoplanets orbiting this star.

N Centauri is a binary star in the southern constellation of Centaurus. The brighter star is dimly visible to the naked eye with an apparent visual magnitude of 5.26, and it is approximately 304 light years away based on parallax. It has an absolute magnitude of +0.76 and is drifting further away from the Sun with a radial velocity of +27 km/s. It is a candidate member of the Sco OB2 moving group.

<span class="mw-page-title-main">HD 136118</span> Star in the constellation Serpens

HD 136118 is a star in the Serpens Caput section of the Serpens constellation. The star is too dim to be readily visible to the naked eye, having an apparent visual magnitude of 6.93. It is located at a distance of 165 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −3 km/s.

Gliese 412 is a pair of stars that share a common proper motion through space and are thought to form a binary star system. The pair have an angular separation of 31.4″ at a position angle of 126.1°. They are located 15.8 light-years distant from the Sun in the constellation Ursa Major. Both components are relatively dim red dwarf stars.

HR 6806 or HD 166620 is a solitary, orange, main sequence, and Sun-like star located thirty-six light-years away, in the constellation Hercules. The star is smaller than the Sun, with around 79% of the solar mass and radius, and 35% of the solar luminosity. It appears to be rotating slowly with an estimated period of 42 days. In 1988, it was noticed that the star had an inactive chromosphere, with a surface magnetic field strength of only 1,500 G. From 1990 activity in the chromosphere increased, inline with a 16 year stellar cycle previously observed. But, sometime after 1994 chromospheric activity greatly reduced, and has stayed flat for more than 16 years. As of 2022, the star appears to have entered the equivalent of a Maunder minimum. The star is around six billion years of age.

<span class="mw-page-title-main">FK Comae Berenices</span> Star in the constellation of Coma Berenices

FK Comae Berenices is a variable star that varies in apparent magnitude between 8.14 and 8.33 over a period of 2.4 days. It is the prototype for the FK Comae Berenices class of variable stars. The variability of FK Com stars may be caused by large, cool spots on the rotating surfaces of the stars. This star is thought to be the result of a recent binary merger, resulting in a high rate of both spin and magnetic activity.

<span class="mw-page-title-main">LN Andromedae</span> Star in the constellation Andromeda

LN Andromedae, also known as HD 217811, HR 8768, is a formerly suspected variable star in the constellation Andromeda. Located approximately 458 parsecs (1,490 ly) away from Earth, it shines with an apparent visual magnitude 6.41, thus it can be seen by the naked eye under very favourable conditions. Its spectral classification is B2V, meaning that it's a hot main sequence star, emitting light approximately with a blackbody spectrum at an effective temperature of 18,090 K.

<span class="mw-page-title-main">LP Aquarii</span> Star in the constellation Aquarius

LP Aquarii is a pulsating variable star in the constellation of Aquarius that varies between magnitudes 6.30 and 6.64. The position of the star near the ecliptic means it is subject to lunar occultations.

HAT-P-4 is a wide binary star consisting of a pair of G-type main-sequence stars in the constellation of Boötes. It is also designated BD+36°2593.

2 Vulpeculae is a binary star system in the northern constellation of Vulpecula, located around 1,800 light years away from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.43.

Gliese 754 is a dim star in the southern constellation of Telescopium. It has an apparent visual magnitude of 12.25, which requires a telescope to view. The star is located at a distance of 19.3 light-years from the Sun based on parallax, and it is drifting further away with a radial velocity of +7 km/s. It is one of the hundred closest stars to the Solar System. Calculations of its orbit around the Milky Way showed that it is eccentric, and indicate that it might be a thick disk object.

<span class="mw-page-title-main">GW Orionis</span> Star in the constellation Orion

GW Orionis is a T Tauri type pre-main sequence hierarchical triple star system. It is associated with the Lambda Orionis star-forming region and has an extended circumtrinary protoplanetary disk.

<span class="mw-page-title-main">HD 111395</span> Star in the constellation Coma Berenices

HD 111395 is a single, variable star in the northern constellation of Coma Berenices. It has the variable star designation LW Com, short for LW Comae Berenices; HD 111395 is the Henry Draper Catalogue designation. The star has a yellow hue and is just bright enough to be barely visible to the naked eye with an apparent visual magnitude that fluctuates around 6.29. Based upon parallax measurements, it is located at a distance of 55.8 light years from the Sun. The star is drifting closer with a radial velocity of −8.9 km/s. It is a member of the Eta Chamaeleontis stellar kinematic group.

HD 99706 is an orange-hued star in the northern circumpolar constellation of Ursa Major. With an apparent visual magnitude of 7.65, it is too dim to be visible to the naked eye but can be viewed with a pair of binoculars. Parallax measurements provide a distance estimate of approximately 480 light years from the Sun, and the Doppler shift shows it is drifting closer with a radial velocity of −30 km/s. It has an absolute magnitude of 2.12, indicating it would be visible to the naked eye as a 2nd magnitude star if it were located 10 parsecs away.

<span class="mw-page-title-main">RW Aurigae</span> Young binary star system in the constellation Auriga

RW Aurigae is a young binary system in the constellation of Auriga about 530 light years away, belonging to the Taurus-Auriga association of the Taurus Molecular Cloud. RW Aurigae B was discovered in 1944.

HD 72945 and HD 72946 form a co-moving star system in the northern constellation of Cancer. HD 72945 is a binary star that is dimly visible to the naked eye as a point of light with an apparent visual magnitude of 5.91. At an angular separation of 10.10″ is the fainter companion star HD 72946 at magnitude 7.25. It is being orbited by a brown dwarf. The system as a whole is located at a distance of approximately 84 light years from the Sun based on parallax measurements.

References

  1. ↑ Starr, Michelle (28 September 2019). "Astronomers Have Found Another 21 Stars Dimming as Erratically as Tabby's Star". ScienceAlert. Retrieved 28 September 2019.
  2. ↑ Schmidt, Edward G. (July 2019). "A Search for Analogs of KIC 8462852 (Boyajian's Star): A Proof of Concept and the First Candidates". The Astrophysical Journal Letters . 880 (1). L7. Bibcode:2019ApJ...880L...7S. doi: 10.3847/2041-8213/ab2e77 . S2CID   199676552.
  3. 1 2 3 4 Way, Z.; et al. (11 September 2020). "ASAS-SN Discovery of a Luminous Star undergoing a Deep Dimming Event". The Astronomer's Telegram . Retrieved 13 September 2020.
  4. 1 2 McCollum, B. & Laine, S. (8 June 2019). "Spectral Type of the Unusual Variable ASASSN-V J213939.3-702817.4". The Astronomer's Telegram . Retrieved 8 June 2019.
  5. 1 2 3 4 Jayasinghe, T.; et al. (4 June 2019). "ASAS-SN Discovery of an Unusual, Deep Dimming Episode of a Previously Non-Variable Star". The Astronomer's Telegram . Retrieved 8 June 2019.
  6. ↑ Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  7. ↑ Nicolet, B. (1978). "Catalogue of Homogeneous Data in the UBV Photoelectric Photometric System". Astronomy & Astrophysics. 34: 1–49. Bibcode:1978A&AS...34....1N.
  8. 1 2 van Leeuwen, F (November 2007). "Hipparcos, the New Reduction". Astronomy and Astrophysics. VizieR. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600.
  9. ↑ "Dimming Betelgeuse likely isn't cold, just dusty, new study shows" (Press release). University of Washington. 6 March 2020. Retrieved 6 March 2020– via EurekAlert!.
  10. ↑ Levesque, Emily M.; Massey, Philip (24 February 2020). "Betelgeuse just isn't that cool: Effective temperature alone cannot explain the recent dimming of Betelgeuse". The Astrophysical Journal Letters. 891 (2). L37. arXiv: 2002.10463 . Bibcode: 2020ApJ...891L..37L . doi: 10.3847/2041-8213/ab7935 . S2CID   211296241.
  11. ↑ Bouy, H. & Martín, Eduardo L. (September 2009). "Proper motions of cool and ultracool candidate members in the Upper Scorpius OB association". Astronomy and Astrophysics. 504 (3): 981–990. arXiv: 0907.0149 . Bibcode:2009A&A...504..981B. doi:10.1051/0004-6361/200811088. S2CID   14150392.
  12. ↑ Preibisch, Thomas; et al. (July 2002). "Exploring the Full Stellar Population of the Upper Scorpius OB Association". The Astronomical Journal. 124 (1): 404–416. Bibcode:2002AJ....124..404P. doi: 10.1086/341174 .
  13. 1 2 Zacharias, N.; et al. (2003). "VizieR Online Data Catalog: The Second U.S. Naval Observatory CCD Astrograph Catalog (UCAC2)". CDS/ADC Collection of Electronic Catalogues (1289). Bibcode:2003yCat.1289....0Z.
  14. 1 2 Rappaport, S.; et al. (May 2019). "Deep Long Asymmetric Occultation in EPIC 204376071" (PDF). Monthly Notices of the Royal Astronomical Society . 485 (2): 2681–2693. arXiv: 1902.08152 . Bibcode:2019MNRAS.485.2681R. doi:10.1093/mnras/stz537. S2CID   119470865.
  15. 1 2 "EPIC 204376071". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 6 March 2019.
  16. ↑ Høg, E.; et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
  17. 1 2 3 4 "EPIC Search Results - EPIC 249706694". Space Telescope Science Institute . Retrieved 12 July 2019.
  18. ↑ Mann, Adam (3 July 2019). "Astronomers Don't Know What to Make of This Incredibly Bizarre Star". Scientific American . Retrieved 3 July 2019.
  19. ↑ Hamilton, Catrina M.; et al. (2001). "Eclipses by a Circumstellar Dust Feature in the Pre-main-Sequence Star KH 15D". The Astronomical Journal. 554 (2): L201–L204. arXiv: astro-ph/0105412 . Bibcode:2001ApJ...554L.201H. doi:10.1086/321707. S2CID   17956137.
  20. ↑ "V582 Monocerotis". The International Variable Star Index. American Association of Variable Star Observers. Retrieved 29 June 2018.
  21. ↑ Aronow, Rachel A.; et al. (2018). "Optical and Radio Observations of the T Tauri Binary KH 15D (V582 Mon): Stellar Properties, Disk Mass Limit, and Discovery of a CO Outflow". The Astronomical Journal. 155 (1): 47. arXiv: 1711.11434 . Bibcode:2018AJ....155...47A. doi: 10.3847/1538-3881/aa9ed7 . S2CID   59444726.
  22. 1 2 Dahm, S. E. & Simon, Theodore (February 2005). "The T Tauri Star Population of the Young Cluster NGC 2264". The Astronomical Journal. 129 (2): 829–855. Bibcode:2005AJ....129..829D. doi: 10.1086/426326 .
  23. ↑ Bailer-Jones, C. A. L.; et al. (August 2018). "Estimating distances from parallaxes IV: Distances to 1.33 billion stars in Gaia Data Release 2". The Astronomical Journal. 156 (2). 58. arXiv: 1804.10121 . Bibcode:2018AJ....156...58B. doi: 10.3847/1538-3881/aacb21 . S2CID   119289017.
  24. 1 2 "HD 181469". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 12 July 2019.
  25. 1 2 3 4 5 6 Osborn, H. P.; et al. (October 2017). "Periodic Eclipses of the Young Star PDS 110 Discovered with WASP and KELT Photometry". Monthly Notices of the Royal Astronomical Society. 471 (1): 740–749. arXiv: 1705.10346 . Bibcode:2017MNRAS.471..740O. doi:10.1093/mnras/stx1249. S2CID   119450480.
  26. ↑ Keenan, Philip C.; McNeil, Raymond C. (1 October 1989). "The Perkins Catalog of Revised MK Types for the Cooler Stars". The Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373. ISSN   0067-0049.
  27. ↑ Watson, C. L. (2006). "The International Variable Star Index (VSX)". The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23–25. 25: 47. Bibcode:2006SASS...25...47W.
  28. 1 2 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR .
  29. ↑ Parker, Richard J.; Crowther, Paul A.; Rate, Gemma (2020). "Unlocking Galactic Wolf–Rayet stars with Gaia DR2 – II. Cluster and association membership". Monthly Notices of the Royal Astronomical Society. 495 (1): 1209–1226. arXiv: 2005.02533 . Bibcode:2020MNRAS.495.1209R. doi:10.1093/mnras/staa1290. S2CID   218516882.
  30. 1 2 Samus, N. N.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog . Bibcode:2009yCat....102025S.
  31. 1 2 "V* RZ Psc". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 22 December 2017.
  32. ↑ Paez, Danny (21 December 2017). "This "Winking" Star is So Hungry it's Feasting on Planets - An appetite of galactic proportions". Inverse innovation . Retrieved 21 December 2017.
  33. 1 2 3 4 5 Boyajian, T. S.; et al. (April 2016). "Planet Hunters IX. KIC 8462852 – where's the flux?". Monthly Notices of the Royal Astronomical Society . 457 (4): 3988–4004. arXiv: 1509.03622 . Bibcode:2016MNRAS.457.3988B. doi:10.1093/mnras/stw218. S2CID   54859232.
  34. 1 2 Masi, Gianluca (16 October 2015). "KIC 8462852: A star and its secrets". The Virtual Telescope Project 2.0. Retrieved 22 October 2015.
  35. ↑ Harvard-Smithsonian Center for Astrophysics (3 January 2022). "Astronomers find mysterious dusty object orbiting a star". Phys.org . Retrieved 3 January 2022.
  36. ↑ Powell, Brian P.; et al. (8 December 2021). "Mysterious Dust-emitting Object Orbiting TIC 400799224". The Astronomical Journal . 162 (6): 299. arXiv: 2110.01019 . Bibcode:2021AJ....162..299P. doi: 10.3847/1538-3881/ac2c81 . S2CID   238259420.
  37. 1 2 3 4 Mamajek, Eric E.; et al. (March 2012). "Planetary Construction Zones in Occultation: Discovery of an Extrasolar Ring System Transiting a Young Sun-like Star and Future Prospects for Detecting Eclipses by Circumsecondary and Circumplanetary Disks". The Astronomical Journal . 143 (3): 72. arXiv: 1108.4070 . Bibcode:2012AJ....143...72M. doi:10.1088/0004-6256/143/3/72. S2CID   55818711.
  38. ↑ Kenworthy, Matthew A. & Mamajek, Eric E. (22 January 2015). "Modeling giant extrasolar ring systems in eclipse and the case of J1407b: sculpting by exomoons?". The Astrophysical Journal. 800 (2): 126. arXiv: 1501.05652 . Bibcode:2015ApJ...800..126K. doi:10.1088/0004-637X/800/2/126. S2CID   56118870.
  39. 1 2 3 4 Saito, Roberto K.; et al. (6 November 2018). "VVV-WIT-07: another Boyajian's star or a Mamajek's object?". Monthly Notices of the Royal Astronomical Society. 482 (4): 5000–5006. arXiv: 1811.02265 . Bibcode:2019MNRAS.482.5000S. doi:10.1093/mnras/sty3004. S2CID   119068259.
  40. 1 2 3 "WD 1145+017". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 25 October 2015.
  41. ↑ "Planet WD 1145+017 b". Extrasolar Planets Encyclopaedia . Retrieved 30 October 2015.
  42. ↑ Pulliam, Christine (21 October 2015). "Cosmic "Death Star" is Destroying a Planet". Harvard-Smithsonian Center for Astrophysics. 2015–21.
  43. 1 2 3 Vanderbosch, Z.; et al. (26 August 2019). "A White Dwarf with Transiting Circumstellar Material Far Outside Its Tidal Disruption Radius". arXiv: 1908.09839v1 [astro-ph.SR].
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