pi Pavonis
{{Short description|Binary star in the constellation Pavo}}
{{Starbox begin}}
{{Starbox image
| image =
{{Location mark
|image=Pavo constellation map.svg|alt=|float=center|width=280
|label=|position=right
|mark=Red circle.svg|mark_width=10|mark_link=Pi Pavonis
|x=745|y=285
}}
| caption = Location of π Pavonis (circled)
}}
{{Starbox observe
| epoch = J2000
| constell = Pavo
| dec = {{DEC|-63|40|06.7906}}
}}
{{Starbox character
| type =
| class = kA4hF0mF2 III + KV
| variable =
}}
{{Starbox astrometry
| parallax = 25.09
| p_error = 0.17
}}
{{Starbox detail
| component1 = A
| mass = 1.80
| radius = 2.80
| age_gyr = 1.4
| luminosity = {{Val|24.69|0.36}}
| temperature = 7,560
| component2 = B
| mass2 = 0.76
| radius2 = 0.70
| temperature2 = 4,710
}}
{{Starbox relpos
|primary = A
| component = B
| projsep = 39.3
| angdistmas = 959
}}
{{Starbox catalog
| names = {{odlist | B=π Pav | CPD=−63°4292 | FK5=3437 | HD=165040 | HIP=88866 | HR=6745 | SAO=254147 | GC=24665 }}
}}
{{Starbox reference
| Simbad = Pi+Pavonis
}}
{{Starbox end}}
π Pavonis, Latinized as Pi Pavonis, is a binary star in the constellation Pavo. It is a white-hued star that is visible to the naked eye as a faint point of light with an apparent visual magnitude of 4.33. The distance to this object is 130 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −15.6 km/s.
The primary component is an chemically peculiar star that displays an abundance anomaly of strontium. Grey et al. (1989) classify it as kA4hF0mF2 III, matching a giant Am star with the calcium K line of an A4 star, the hydrogen lines of a cooler F0 star, and the metal lines of a F2 star. However, Loden and Sundman (1989) don't consider it to be a giant and list it as an Ap star. It is 1.4 billion years old with 1.8 times the mass of the Sun and 2.8 times the Sun's radius. The star is radiating 24.7 times the Sun's luminosity from its photosphere at an effective temperature of 7,560 K.
The secondary is a K-type main-sequence star, much smaller than its primary, at 0.76 solar masses and 0.7 solar radii. It has an effective temperature 4,710 K and is 3.63 magnitudes fainter than the primary in the H band. They are separated by 39.3 astronomical units and have an estimated orbital period of 150 years.
There is evidence for a more distant companion using Hipparcos-Gaia astrometry, which should be a star with less than 0.7 times the mass of the Sun, closer to the primary star.
References
{{reflist|refs=
{{cite simbad | title=pi Pav | access-date=2019-10-12 }}
{{cite DR2|6630558558672843392}}
| title=Automated spectroscopic abundances of A and F-type stars using echelle spectrographs. II. Abundances of 140 A-F stars from ELODIE
| last1=Erspamer | first1=D. | last2=North | first2=P.
| journal=Astronomy and Astrophysics
| volume=398 | pages=1121–1135 | date=February 2003
| issue=3 | arxiv=astro-ph/0210065 | bibcode=2003A&A...398.1121E
| doi=10.1051/0004-6361:20021711 | s2cid=1109164 }}
| title=Giant CP stars?
| last1=Loden | first1=L. O. | last2=Sundman | first2=A.
| journal=Journal of Astrophysics and Astronomy
| volume=10 | pages=183–196 | date=June 1989
| issue=2 | doi=10.1007/BF02719315 | bibcode=1989JApA...10..183L | s2cid=121258394 }}
{{cite journal | last=Wilson | first=R. E. | year=1953 | title=General Catalogue of Stellar Radial Velocities | journal=Carnegie Institute Washington D.C. Publication | publisher=Carnegie Institution of Washington | bibcode=1953GCRV..C......0W | lccn=54001336 }}
}}
{{Stars of Pavo}}
{{DEFAULTSORT:Pi Pavonis}}