Pi Pavonis

π Pavonis, Latinized as Pi Pavonis, is a binary star^[4] 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.^[2] The distance to this object is 130 light years based on parallax,^[1] but it is drifting closer to the Sun with a radial velocity of −15.6 km/s.^[6]

Pi Pavonis

Location of π Pavonis (circled)
Observation data Epoch J2000      Equinox J2000
Constellation	Pavo
Right ascension	18h 08m 34.81459s[1]
Declination	−63° 40′ 06.7906″[1]
Apparent magnitude (V)	4.33[2]
Characteristics
Spectral type	kA4hF0mF2 III[3] + KV[4]
U−B color index	+0.17[5]
B−V color index	+0.23[5]
Astrometry
Radial velocity (Rv)	−15.60[6] km/s
Proper motion (μ)	RA: +18.02[1] mas/yr Dec.: -207.57[1] mas/yr
Parallax (π)	25.09±0.17 mas[1]
Distance	130.0 ± 0.9 ly (39.9 ± 0.3 pc)
Absolute magnitude (MV)	1.33[2]
Details[4]
A
Mass	1.80 M☉
Radius	2.80 R☉
Luminosity	24.69±0.36[7] L☉
Surface gravity (log g)	3.81[8] cgs
Temperature	7,560 K
Metallicity [Fe/H]	0.27[8] dex
Rotational velocity (v sin i)	30.0[9] km/s
Age	1.4 Gyr
B
Mass	0.76 M☉
Radius	0.70 R☉
Temperature	4,710 K
Position (relative to A)[4]
Component	B
Angular distance	959 mas
Projected separation	39.3 AU
Other designations
π Pav, CPD−63°4292, FK5 3437, GC 24665, HD 165040, HIP 88866, HR 6745, SAO 254147[10]
Database references
SIMBAD	data

The primary component is an chemically peculiar star that displays an abundance anomaly of strontium.^[11][12] Grey et al. (1989) classify it as kA4hF0mF2 III,^[3] 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.^[11] It is 1.4 billion years old with 1.8 times the mass of the Sun and 2.8 times the Sun's radius.^[4] The star is radiating 24.7^[7] times the Sun's luminosity from its photosphere at an effective temperature of 7,560 K.^[4]

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.^[4]

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.^[4]