It bore the traditional name Tureis or Turais, from the
Arabicتُرَيْسturays "shield" (
diminutive), which was shared by
Iota Carinae.[16] In 2016, the
International Astronomical Union organized a
Working Group on Star Names (WGSN)[17] to catalogue and standardize proper names for stars. The WGSN approved the name Tureis for this star on 12 September 2016 and it is now so entered in the IAU Catalog of Star Names (Iota Carinae was given the name Aspidiske on 20 July 2016).[15]
Properties
At present Rho Puppis is moving away from the Sun with a
radial velocity of +46.1 km s−1. The closest approach occurred about 394,000 years ago when it came within roughly 11.6 ly (3.6 pc) of the
Solar System; about the same distance as
Procyon in the present era.[19]
The
variability of this star was announced in 1956 by American astronomer
Olin J. Eggen.[5] It was determined to be a
Delta Scuti-type variable star, making it one of the first stars of that type to be identified. Photometric observations dating back to 1946 provide a lengthy record of its pattern of pulsation; it undergoes periodic pulsations with a single period of 0.14088143(3) days,[20] or 7.1 cycles per day. During each cycle, the star's magnitude varies with an amplitude of 0.15 and the radial velocity varies by 10 km s−1. The peak brightness occurs 28.8 minutes following the minimum radial velocity.[5] The
outer atmosphere'seffective temperature of 6,920 K[11] is one of the lowest known for a Delta Scuti variable.[5]
Rho Puppis has an estimated age of about 2 billion years[13] and it has 3.4[9] times the Sun's radius. It has a stellar classification of F5IIkF2IImF5II.[4] This complex format indicates that ρ Puppis is an Am star, with relatively weak lines of calcium and strong lines of other metals. The spectral type indicated by the calcium k line is F5, while that indicated by heavier metal
absorption lines is F2. The roman numerals indicate a
luminosity class of
bright giant. Most such stars are found in binary star systems,[21] but this appears to be an exception as no companion has been discovered.[13][22] Evolved stars with Am-like peculiarities of abundance have come to be known as ρ Puppis stars.[23] The star's
metallicity is more than double that in the Sun.[10]
This star shows an
excess emission of infrared radiation, suggesting that there is a circumstellar
disk of dust orbiting this star. The mean temperature of the emission is 85 K, corresponding to an orbital separation from the host star of 50
AU.[9][13]
^
abcdBookmeyer, B. B.; et al. (August 1977), "Photoelectric UBV observations of RR Lyrae variable stars. Second list", Revista Mexicana de Astronomía y Astrofísica, 2: 235–258,
Bibcode:
1977RMxAA...2..235B
^
abGray, R. O; Corbally, C. J; Garrison, R. F; McFadden, M. T; Robinson, P. E (2003), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I", The Astronomical Journal, 126 (4): 2048,
arXiv:astro-ph/0308182,
Bibcode:
2003AJ....126.2048G,
doi:
10.1086/378365,
S2CID119417105
^
abcdMathias, P.; et al. (November 1997), "A spectroscopic study of the delta Scuti star rho Puppis", Astronomy and Astrophysics, 327: 1077–1086,
Bibcode:
1997A&A...327.1077M
^Evans, D. S. (June 20–24, 1966), Batten, Alan Henry; Heard, John Frederick (eds.), "The Revision of the General Catalogue of Radial Velocities", Determination of Radial Velocities and Their Applications, Proceedings from IAU Symposium No. 30, 30, University of Toronto: International Astronomical Union: 57,
Bibcode:
1967IAUS...30...57E
^
abcBurkhart, C.; Coupry, M. F. (September 1991), "The A and Am-Fm stars. I - The abundances of Li, Al, Si, and Fe", Astronomy and Astrophysics, 249 (1): 205–216,
Bibcode:
1991A&A...249..205B
^Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago, 239 (1): 1,
Bibcode:
1970CoAsi.239....1B
^Moon, T.; van Antwerpen, C. (June 2009), "Period Changes in δ Scuti Stars: ρ Puppis", The Journal of the American Association of Variable Star Observers, 37 (1): 3–14,
Bibcode:
2009JAVSO..37....3M