List of stars that dim oddly

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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 dim oddly is a table of stars that have been observed to darken and brighten and don't appear to be eclipsing binaries or intrinsic variables. It's 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
RZ Piscium K0 IV [26] 11.29–13.82 [26] —01h 09m 42.056s [27] +27° 57′ 1.95″ [27] 550 [28] Substantial mass of gas and dust, possibly from disrupted planet
Tabby's Star
(KIC 8462852)		F3V [29] [30] 11.705 [30] 3.08 [29] 20h 06m 15.4527s [29] +44° 27′ 24.791″ [29] 1470 [29] Unknown
TIC 400799224 ——————"probably from an orbiting body that periodically emits clouds of dust that occult the star" [31] [32]
V1400 Centauri K5 IV(e) Li [33] 12.31 [33] —14h 07m 47.93s [33] −39° 45′ 42.7″ [33] 434 [34] Planet with gigantic ring system
VVV-WIT-07 —14.35–16.164 [35] —17h 26m 29.387s [35] −35° 40′ 6.20″ [35] 23000/? [35] Unknown
WD 1145+017
(EPIC 201563164)		DB [36] 17.0 [37] —11h 48m 33.63s [36] +01° 28′ 59.4″ [36] 570 [38] Dust disk
ZTF J0139+5245
(ZTF J013906.17+524536.89)		DA [39] 18.4 [39] —01h 39m 06.17s+52° 45′ 36.89″564 [39] Dust disk

See also

Related Research Articles

4 Andromedae, abbreviated 4 And, is a single star in the northern constellation of Andromeda. 4 Andromedae is the Flamsteed designation. It is dimly visible to the naked eye with an apparent visual magnitude of 5.308. Based upon an annual parallax shift of 9.7 mas as seen from Earth's orbit, it is located 337 light years away. The star is moving closer with a heliocentric radial velocity of −11 km/s. It has a magnitude 11.7 visual companion at an angular separation of 51.10″ along a position angle of 348°, as of 2002.

77 Aquarii is a single star located 135 light years away from the Sun in the equatorial constellation of Aquarius. 77 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim star with a baseline apparent visual magnitude of 5.55. The star is moving closer to the Earth with a heliocentric radial velocity of −35 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 patallax 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.

HD 69863 is a binary star system in the southern constellation of Carina. It is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.16. The system is located at a distance of about255 light years from the Sun based on parallax. The dual nature of this system was announced in 1832 by German astronomer Carl Rümker. As of 2015, the pair had an angular separation of 4.10″ along a position angle of 70°.

42 Cassiopeiae is a possible binary star system in the northern circumpolar constellation of Cassiopeia. It is visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of +5.18. The system is located approximately 291 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +7 km/s.

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.

EQ Virginis Star in the constellation Virgo

EQ Virginis is a single variable star in the equatorial constellation of Virgo. It has a baseline visual apparent magnitude of 9.36, but is a flare star that undergoes sporadic bursts of brightening. The star is located at a distance of 67 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −23 km/s. It is a member of the IC 2391 moving group of stars, which is between 30 and 50 million years old.

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.

Gamma Doradus, Latinized from γ Doradus, is the third-brightest star in the southern constellation of Dorado. It is faintly visible to the naked eye with an apparent visual magnitude of approximately 4.25, and is a variable star, the prototype of the class of Gamma Doradus variables. The star is located at a distance of 67 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +25 km/s. Based on its motion through space, it appears to be a member of the IC 2391 supercluster.

GJ 3379 is the nearest star in the Orion constellation, located at a distance of 17 light years from the Sun based on parallax. It is a single star with an apparent visual magnitude of +11.31 and an absolute magnitude of +12.71, therefore, the star is not visible with the naked eye. It is positioned in the upper left part of the Orion constellation, to the SSE of Betelgeuse. This star is drifting further away with a radial velocity of +30.0 kilometers per second. In the past, this star had a relatively close encounter with the Solar System. Some 161,000±6,000 years ago, it achieved a minimum distance of 4.08 ± 0.20 ly (1.25 ± 0.06 pc).

Gliese 752 Star in the constellation Aquila

Gliese 752 is a binary star system in the Aquila constellation. This system is relatively nearby, at a distance of about 19 light years. This system consists of two M-type stars. The primary star is the magnitude 9 Gliese (GJ) 752 A. The secondary star is the dim magnitude 17 Gliese (GJ) 752 B, more commonly referred to as VB 10. This stellar pair form a binary star system separated by about 74 arc seconds. This system is also known for its high proper motion of about 1 arc second a year.

25 Orionis Star in the constellation Orion

25 Orionis, less commonly known by its Bayer designation Psi1 Orionis is a fifth-magnitude star in the constellation Orion. It lies among a dense cluster of low-mass pre-main-sequence stars in the Orion OB1a.

μ Cygni, Latinised as Mu Cygni, is a binary star system in the northern constellation of Cygnus. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.49. The system is located 72 light years distant from the Sun, based on parallax, and is drifting further away with a radial velocity of +17 km/s.

Nu Fornacis, Latinized from ν Fornacis, is a single, variable star in the southern constellation of Fornax. It is blue-white in hue and faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.69. This body is located approximately 370 light years distant from the Sun based on parallax, and is drifting further away with a radial velocity of +18.5 km/s. It is a candidate member of the Pisces-Eridanus stellar stream, which suggests an age of 120 million years or less.

Exocomet Comet outside the Solar System

An exocomet, or extrasolar comet, is a comet outside the Solar System, which includes rogue comets and comets that orbit stars other than the Sun. The first exocomets were detected in 1987 around Beta Pictoris, a very young A-type main-sequence star. There are now a total of 27 stars around which exocomets have been observed or suspected.

8 Persei is a single star in the northern constellation of Perseus, located 416 light years away from the Sun. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.757. There is an estimated 52% chance that the star may be a member of the Hyades–Pleiades stream of co-moving stars.

Tabbys Star Star noted for unusual dimming events

Tabby's Star is an F-type main-sequence star in the constellation Cygnus approximately 1,470 light-years from Earth. Unusual light fluctuations of the star, including up to a 22% dimming in brightness, were discovered by citizen scientists as part of the Planet Hunters project. In September 2015, astronomers and citizen scientists associated with the project posted a preprint of an article describing the data and possible interpretations. The discovery was made from data collected by the Kepler space telescope, which observed changes in the brightness of distant stars to detect exoplanets.

Disrupted planet Planet or related being destroyed by a passing object

In astronomy, a disrupted planet is a planet or exoplanet or, perhaps on a somewhat smaller scale, a planetesimal, moon, exomoon or asteroid that has been disrupted or destroyed by a nearby or passing astronomical body or object such as a star. Necroplanetology is the related study of such a process. Nonetheless, the result of such a disruption may be the production of excessive amounts of related gas, dust and debris, which may eventually surround the parent star in the form of a circumstellar disk or debris disk. As a consequence, the orbiting debris field may be an "uneven ring of dust", causing erratic light fluctuations in the apparent luminosity of the parent star, as may have been responsible for the oddly flickering light curves associated with the starlight observed from certain variable stars, such as that from Tabby's Star, RZ Piscium and WD 1145+017. Excessive amounts of infrared radiation may be detected from such stars, suggestive evidence in itself that dust and debris may be orbiting the stars.

RW Aurigae 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. 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.
  27. 1 2 "V* RZ Psc". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 22 December 2017.
  28. ↑ 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.
  29. 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.
  30. 1 2 Masi, Gianluca (16 October 2015). "KIC 8462852: A star and its secrets". The Virtual Telescope Project 2.0. Retrieved 22 October 2015.
  31. ↑ Harvard-Smithsonian Center for Astrophysics (3 January 2022). "Astronomers find mysterious dusty object orbiting a star". Phys.org . Retrieved 3 January 2022.
  32. ↑ 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 . Retrieved 4 January 2022.
  33. 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.
  34. ↑ 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.
  35. 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.
  36. 1 2 3 "WD 1145+017". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 25 October 2015.
  37. ↑ "Planet WD 1145+017 b". The Extrasolar Planet Encyclopedia. Retrieved 30 October 2015.
  38. ↑ Pulliam, Christine (21 October 2015). "Cosmic "Death Star" is Destroying a Planet". Harvard-Smithsonian Center for Astrophysics. 2015–21.
  39. 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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