Delta Pavonis
Delta Pavonis is a single star in the southern constellation of Pavo. Its name is a Bayer designation that is Latinized from δ Pavonis, and abbreviated Delta Pav or δ Pav. It has an apparent visual magnitude of 3.56, making it a fourth-magnitude star that is visible to the naked eye from the southern hemisphere. Parallax measurements yield an estimated distance of from Earth. This makes it one of the nearest bright stars to the Solar System. It is approaching the Sun with a radial velocity of −23.5 km/s, and is predicted to come as close as in around 49,200 years.
Physical characteristics
This object is a subgiant of spectral type G8 IV; it will stop fusing hydrogen at its core relatively soon, starting the process of becoming a red giant. Hence, Delta Pavonis is 24% brighter than the Sun, but the effective temperature of its outer atmosphere is less: 5,571 K. Its mass is 107% of Sun's mass, with a radius 120% of Sun's radius. Delta Pavonis's surface convection zone extends downward to about 43.1% of the star's radius, but only contains 4.8% of the star's mass.Spectroscopic examination of Delta Pavonis shows that it has a higher abundance of elements heavier than helium than does the Sun. This value is typically given in terms of the ratio of iron to hydrogen in a star's atmosphere, relative to that in Sun's atmosphere. The metallicity of Delta Pavonis is approximately
This notation gives the logarithm of the iron-to-hydrogen ratio, relative to that of the Sun, meaning that Delta Pavonis's iron abundance is 235% of that of Sun. It is considered super metal-rich, and the high metallicity has slowed its evolution. Studies have shown a correlation between abundant heavy elements in stars, and the presence of a planetary system, so Delta Pavonis has a greater than average probability of harboring planets.
The age of Delta Pavonis is approximately 6.1 billion years. It has a projected rotational velocity of 0.32 kilometers per second, and is spinning with of roughly 21 days, slightly faster than the Sun.