RR Pictoris

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Double star
RR Pictoris
AladinLite
Observation
dates equinox :  J2000.0 , epoch : J2000.0
Constellation painter
Right ascension 6 h 35 m 36.25 s
declination -62 ° 38 ′ 22 ″
Apparent brightness 1.0 - 12.9 mag
Typing
rel. Brightness
(G-band) 		(12.407 ± 0.005) mag
rel. Brightness
(J-band) 		(12.458 ± 0.024) mag
B − V color index −0.202 
Spectral class Q
Variable star type NB 
Astrometry
parallax (1.9554 ± 0.0304)  mas
distance 1,696  ly
520  pc  
Proper movement 
Rec. Share: (3.362 ± 0.122)  mas / a
Dec. portion: (−3.579 ± 0.124)  mas / a
Physical Properties
Rotation time 3.48 h
Other names
and catalog entries
2MASS catalog 2MASS J06353606-6238242 [1]
Other names Nova Pic 1925, RR Pic, HIP 31481, ASAS J063536-6238.3, CSI-62-06352, 2E 1715, HIC 31481, PLX 1557, AAVSO 0634-62, Gaia DR1 5477422095246244224

Template: Infobox star / maintenance / magGTemplate: Infobox star / maintenance / magJ

RR Pictoris , also Nova Pictoris 1925 , was a slowNB type Nova thatlit upin the painter constellation . It was discovered on May 25, 1925 by the South African astronomer R. Watson with a magnitude of 2.3 m . Its brightness continued to increase until it reached its maximum of 1.1 ± 0.1 m on June 6, 1925.

There seems to be enough evidence to suggest that the June 1925 maximum was a secondary event. With the assumption that the primary eruption had reached at least the same magnitude as the maximum in June and would have been observed sometime after February 18, the brightness could and would have dropped to 3.0 m on April 13, 1925 thus clearly better match a required linear decrease of t2 = 29 days.

The brightness continued to decrease to 4.0 m by July 4, but rose again to 1.9 m on August 9 . Half a year after the maximum, RR Pictoris faded so much that it was no longer visible to the naked eye, and by 1975 it had decreased to a magnitude of 12.5 m .

RR Pictoris is a cataclysmically variable binary star system consisting of a companion star that has crossed its Roche limit and a white dwarf that orbit each other in close orbit with a period of 3.48 hours. Speed ​​calculations indicate that the companion is no longer on the main row and has already started to puff up and cool down as hydrogen fusion in the core has stalled. The distance from RR-Pictoris to the earth is estimated to be about 520 pc (1,696 ly ).

Individual evidence

  1. ↑ a b c d e f V * RR Pic. In: SIMBAD . Center de Données astronomiques de Strasbourg , accessed April 4, 2019 .
  2. ↑ a b c RR Pic. In: VSX. AAVSO , accessed April 4, 2019 .
  3. ↑ a b c d Thomas E. Harrison et al .: HST Fine Guidance Sensor Parallaxes for Four Classical Novae . In: The Astrophysical Journal . February 13, 2013. arxiv : 1302.3245 . doi : 10.1088 / 0004-637X / 767/1/7 .
  4. ↑ Some South African Amateur Astronomers. In: Houghton, HE Monthly Notes of the Astronomical Society of South Africa, Vol. 6, p. 45, accessed April 4, 2019 .
  5. ^ Robert Burnham [1977]: Burnham's Celestial Handbook, Volume Three: An Observer's Guide to the Universe Beyond the Solar System . Courier Dover Publications, New York, New York 2013, ISBN 9780486318035 , pp. 1460-62.
  6. ↑ Ribeiro, Fabíola MA: A Tomographic Study of the Classical Nova RR Pictoris . In: Publications of the Astronomical Society of the Pacific . 118, No. 839, 2006, pp. 84-93. arxiv : astro-ph / 0510042 . bibcode : 2006PASP..118 ... 84R . doi : 10.1086 / 498458 .