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RZ Leonis Minoris is a cataclysmic variable star system in the northern constellation of Leo Minor. It undergoes frequent outbursts[5] that vary in brightness from an apparent visual magnitude of 14.4 down to 16.8.[3] Based on parallax measurements, this system is located at a distance of approximately 2,160 light years from the Sun.[2]

RZ Leonis Minoris

A light curve for RZ Leonis Minoris, adapted from Kato et al. (2016)[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Leo Minor
Right ascension 09h 51m 48.926s[2]
Declination 34° 07 23.97[2]
Apparent magnitude (V) 14.4 to 16.8[3]
Characteristics
Variable type Nova-like[3]
Astrometry
Proper motion (μ) RA: −4.848 mas/yr[2]
Dec.: −22.151 mas/yr[2]
Parallax (π)1.5127 ± 0.0335 mas[2]
Distance2,160 ± 50 ly
(660 ± 10 pc)
Other designations
RZ LMi, SDSS J095148.93+340723.8[4]
Database references
SIMBADdata

This system became an object of interest in 1981 when V. A. Lipovetsky and J. A. Stepanian showed it to be a variable star with an ultraviolet excess. It shows strong variation from magnitude 14 down to 17, and the energy distribution at maximum resembles an OB star.[1] The system displays a cyclical light curve, for which J. W. Robertson and colleagues in 1993 found a stable period of 19.2 days.[6] The object differs from most dwarf novae by displaying short-term brightening and fading.[1]

The behavior of the system is similar to ER Ursae Majoris, showing superoutbursts and superhumps. This indicates that RZ LMi is a SU Ursae Majoris-type dwarf novae belonging to the ER UMa sub-class.[1] None of the variation can be linked to the orbital period of this binary system, and thus there is little known about the individual components. The high activity level of this object and the stability of the 19-day supercycle may indicate there is a third body in the system.[5]


References


  1. Kato, Taichi; et al. (December 2016), "RZ Leonis Minoris bridging between ER Ursae Majoris-type dwarf nova and nova-like system", Publications of the Astronomical Society of Japan, 68 (6): 14, arXiv:1609.08791, Bibcode:2016PASJ...68..107K, doi:10.1093/pasj/psw101, 107.
  2. Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  3. Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
  4. "RZ LMi", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2022-05-19.
  5. Olech, A.; Wisniewski, M.; Zloczewski, K.; Cook, L. M.; Mularczyk, K.; Kedzierski, P. (June 2008), "Curious Variables Experiment (CURVE). RZ LMi - the Most Active SU UMa Star", Acta Astronomica, 58: 131–152, arXiv:0806.1657, Bibcode:2008AcA....58..131O.
  6. Robertson, J. W.; et al. (1994), Shafter, Allen W. (ed.), "The Unusual Long-Term Repetitive Light Curve of RZ Leonis Minoris", Interacting binary stars : a symposium held in conjunction with the 105th Meeting of the Astronomical Society of the Pacific, San Diego State University, 13-15 July 1993, San Francisco, Calif: Astronomical Society of the Pacific, vol. 56, p. 298, Bibcode:1994ASPC...56..298R.

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