Wikipedia

RZ Piscium

RZ Piscium (or RZ Psc) is a UX Orionis type variable star[7] 608 light-years (186 pc) away, in the constellation Pisces.[2] Over the years, the star has been found to brighten and dim erratically, dimming by as much as a tenth of its usual luminosity.[11] RZ Piscium has been found to emit large amounts of infrared radiation,[9] suggesting the presence of a substantial mass of gas and dust orbiting the star, possibly from a "disrupted planet".[6][12]

RZ Piscium

Dust and debris orbiting a star (artist's concept)
Observation data
Epoch J2000      Equinox J2000
Constellation Pisces[1]
Right ascension 01h 09m 42.0522s[2]
Declination +27° 57′ 01.910″[2]
Apparent magnitude (V) 11.29 - 13.82[3]
Characteristics
Spectral type K0IV[3]
Variable type UX Ori[3]
Astrometry
Proper motion (μ) RA: 27.544(28) mas/yr[2]
Dec.: −12.521(19) mas/yr[2]
Parallax (π)5.3661 ± 0.0274 mas[2]
Distance608 ± 3 ly
(186.4 ± 1.0 pc)
Details[4]
RZ Piscium A
Radius1.0[5] R☉
Luminosity0.8[5] L☉
Temperature5,600 K (5,330 °C);[6]
5,620 K (5,350 °C);[7]
5,870 K (5,600 °C)[8] K
Age30 − 50[8][9] Myr
RZ Piscium B
Mass0.12 M☉
Other designations
RZ Psc, TYC 1753-1498-1, 2MASS J01094205+2757020[10]
Database references
SIMBADdata

Disrupted planet

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Because of the infrared excess and rapid light variations, astronomers conclude that:

destruction of one or more massive orbiting bodies has recently occurred within 1 au of the star, and we are viewing the aftermath of such an event along the plane of the orbiting debris.[8]

According to astronomer Ben Zuckerman:

Most sun-like stars have lost their planet-forming disks within a few million years of their birth. The fact that RZ Piscium hosts so much gas and dust after tens of millions of years means it is probably destroying, rather than building, planets.[13]

Observations

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A visual band light curve for RZ Piscium, adapted from Shakhovskoǐ et al. (2003)[14]

In 2017, RZ Piscium was studied using the XMM-Newton satellite, the Shane 3-meter telescope at Lick Observatory in California and the 10-meter Keck I telescope at W. M. Keck Observatory in Hawaii.[8][9] The temperature of the star was found to be about the same as the Sun (5,600 K (5,330 °C)).[6] Further, the star was found to produce about a thousand times more x-rays than the Sun, suggesting that the star is relatively young.[6][11] On the other hand, RZ Piscium was found to contain a relatively small amount of surface lithium, which suggests the star is between 30 − 50 million years old; this is somewhat "old" for a star with so much circumstellar dust.[6][11] Most young stars that are as dusty as RZ Piscium may be producing planets, but given its relatively advanced age, RZ Piscium may be destroying and consuming its planets instead.[11]

In 2020, a red dwarf companion with the mass of 0.12 Solar mass was detected with a projected separation of 23 AU from the primary star. The incandescence of the companion star thus make up about one third of excess infrared emission previously attributed to the dust.[4]

See also

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References

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  1. ^ Staff (2008). "Finding the constellation which contains given sky coordinates". djm.com. Retrieved 22 December 2017.
  2. ^ a b c d e 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.
  3. ^ a b c Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  4. ^ a b Sturm, Ardjan; Stolker, Tomas; Rab, Christian; Quiroga-Nuñez, Luis Henry; Milli, Julien; Ménard, François; Kral, Quentin; Van Holstein, Rob G.; Henning, Thomas; Benisty, Myriam; Kenworthy, Matthew A.; Ginski, Christian; Kennedy, Grant M. (2020). "A low-mass stellar companion to the young variable star RZ PSC". Monthly Notices of the Royal Astronomical Society: Letters. 496 (1): L75–L79. arXiv:2005.14203. Bibcode:2020MNRAS.496L..75K. doi:10.1093/mnrasl/slaa092. S2CID 219124422.
  5. ^ a b Su, Kate Y. L.; et al. (1 December 2023). "RZ Piscium Hosts a Compact and Highly Perturbed Debris Disk". The Astrophysical Journal. 959 (1) 43. arXiv:2310.12336. Bibcode:2023ApJ...959...43S. doi:10.3847/1538-4357/ad04d9.
  6. ^ a b c d e Staff (22 December 2017). "Young Star RZ Piscium is 'Eating' Its Own Planets, Astronomers Say". Sci-News.com. Retrieved 22 December 2017.
  7. ^ a b Potravnov, I.S.; et al. (March 2014). "An in-depth analysis of the RZ Piscium atmosphere". Astronomy & Astrophysics. 563: A139. Bibcode:2014A&A...563A.139P. doi:10.1051/0004-6361/201423522.
  8. ^ a b c d Punzi, K. M.; Kastner, J. H.; Melis, C.; Zuckerman, B.; Pilachowski, C.; Gingerich, L.; Knapp, T. (21 December 2017). "Is the Young Star RZ Piscium Consuming Its Own (Planetary) Offspring?". The Astronomical Journal. 155 (1): 33. arXiv:1712.08962. Bibcode:2018AJ....155...33P. doi:10.3847/1538-3881/aa9524. S2CID 119530135.
  9. ^ a b c Reddy, Francis; Garner, Rob (21 December 2017). "New Study Finds 'Winking' Star May Be Devouring Wrecked Planets". NASA. Retrieved 22 December 2017.
  10. ^ "V* RZ Psc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 22 December 2017.
  11. ^ a b c d Byrd, Deborah (22 December 2017). "Is the star RZ Piscium eating its planets?". Earth & Sky. Retrieved 22 December 2017.
  12. ^ Fryling, Kevin (21 December 2017). "IU astronomer's analysis helps discover that a star in the constellation Pisces is a 'planet-eater'". Indiana University. Retrieved 23 December 2017.
  13. ^ 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.
  14. ^ Shakhovskoĭ, D. N.; Grinin, V. P.; Rostopchina, A. N. (July 2003). "Photometric and Polarimetric Activity of RZ Psc". Astronomy Reports. 47 (7): 580–586. Bibcode:2003ARep...47..580S. doi:10.1134/1.1592837. S2CID 123184405. Retrieved 23 February 2022.
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