HD 178322
HD 178322, also known as HR 7257 or rarely 45 G. Coronae Australis, is a double-lined spectroscopic binary located in the southern constellation Corona Australis. It has a combined apparent magnitude of 5.86, making it faintly visible to the naked eye under ideal conditions. The system is located relatively far at a distance of roughly 1,550 light-years based on Gaia DR3 parallax measurements, and it is currently receding with a heliocentric radial velocity of. At its current distance, HD 178322's brightness is diminished by an extinction of 0.28 magnitudes and it has an absolute magnitude of −2.31. The system has a high peculiar velocity of, indicating that it may be a runaway star system; it is said to be part of the Scorpius-Centaurus Association.
The components of HD 178322 are both B-type main-sequence stars with stellar classifications of B5 V and B6 V respectively. Both stars have roughly 4.4 times the mass of the Sun and they spin moderately with projected rotational velocities of. The primary has 3.26 times the radius of the Sun and it radiates 11,749 times the luminosity of the Sun from its photosphere at an effective temperature of. The companion has 3.07 times the Sun's girth and it radiates 513 times the luminosity of the Sun from its photosphere at an effective temperature of. Both stars take roughly 12 days to complete a relatively circular orbit at a separation of. The system is estimated to be 50 million years old.