Iota Coronae Borealis

Iota Coronae Borealis, Latinized from ι Coronae Borealis, is a binary star^[6] system in the constellation Corona Borealis. It is visible to the naked eye with a combined apparent visual magnitude of is 4.96.^[2] Based upon an annual parallax shift of 8.8 mas as seen from the Earth, it is located about 372 light years from the Sun.

ι Coronae Borealis

Observation data Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation	Corona Borealis
Right ascension	16h 01m 26.56492s[1]
Declination	+29° 51′ 03.8194″[1]
Apparent magnitude (V)	4.96[2]
Characteristics
Spectral type	A0 IIIp(HgMnEu)s[3]
U−B color index	−0.15[2]
B−V color index	−0.06[2]
Astrometry
Radial velocity (Rv)	−20.8±0.4[4] km/s
Proper motion (μ)	RA: −38.817[1] mas/yr Dec.: −7.016[1] mas/yr
Parallax (π)	8.7701±0.0857 mas[1]
Distance	372 ± 4 ly (114 ± 1 pc)
Absolute magnitude (MV)	+0.08[5]
Orbit[6]
Period (P)	35.474 d
Eccentricity (e)	0.56
Periastron epoch (T)	2441566.96 JD
Argument of periastron (ω) (secondary)	156°
Semi-amplitude (K1) (primary)	2.3 km/s
Details
ι CrB A
Luminosity	90[7] L☉
Surface gravity (log g)	3.84±0.16[8] cgs
Temperature	10,727±278[8] K
Metallicity [Fe/H]	−0.01±0.12[8] dex
Rotational velocity (v sin i)	18[9] km/s
Other designations
ι CrB, 14 CrB, BD+30°2738, HD 143807, HIP 78493, HR 5971, SAO 84152[10]
Database references
SIMBAD	data

This is a single-lined spectroscopic binary with an orbital period of 35.5 days and an eccentricity of 0.56.^[6] The visible member, component A, has a stellar classification of A0 IIIp(HgMnEu)s,^[3] indicating it is a chemically peculiar mercury-manganese star with narrow absorption lines. The secondary member, component B, appears to be an A-type star.^[11]