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40 Eridani / Keid

Location of 40 Eridani (circled)
Observation data Epoch J2000.0      Equinox J2000.0
Constellation	Eridanus
40 Eridani A
Right ascension	04 15 16.31962
Declination	−07° 39′ 10.3308″
Apparent magnitude (V)	4.43
40 Eridani B
Right ascension	04 15 21.79572
Declination	−07° 39′ 29.2040″
Apparent magnitude (V)	9.52
40 Eridani C
Right ascension	04 15 21.53600
Declination	−07° 39′ 20.6946″
Apparent magnitude (V)	11.17
Characteristics
40 Eridani A
Spectral type	K0.5V
U−B color index	+0.45
B−V color index	+0.82
40 Eridani B
Spectral type	DA4
U−B color index	+0.45
B−V color index	+0.03
40 Eridani C
Spectral type	M4.5eV
U−B color index	+0.83
B−V color index	+1.67
Variable type	Flare star
Astrometry
40 Eridani A
Radial velocity (Rv)	−42.47±0.12 km/s
Proper motion (μ)	RA: −2,240.085 mas/yr Dec.: −3,421.809 mas/yr
Parallax (π)	199.6080 ± 0.1208 mas
Distance	16.340 ± 0.010 ly (5.010 ± 0.003 pc)
Absolute magnitude (MV)	5.93
40 Eridani B
Radial velocity (Rv)	−21 km/s
Proper motion (μ)	RA: −2,236.169 mas/yr Dec.: −3,338.955 mas/yr
Parallax (π)	199.6911 ± 0.0512 mas
Distance	16.333 ± 0.004 ly (5.008 ± 0.001 pc)
40 Eridani C
Radial velocity (Rv)	−44.06±0.20 km/s
Proper motion (μ)	RA: −2,247.183 mas/yr Dec.: −3,409.824 mas/yr
Parallax (π)	199.4516 ± 0.0692 mas
Distance	16.353 ± 0.006 ly (5.014 ± 0.002 pc)
Orbit
Primary	40 Eridani A
Companion	40 Eridani BC
Period (P)	~8,000 yr
Semi-major axis (a)	~400 AU
Orbit
Primary	40 Eridani B
Companion	40 Eridani C
Period (P)	230.30±0.68 yr
Semi-major axis (a)	6.930±0.050" (~35 AU)
Eccentricity (e)	0.4294±0.0027
Inclination (i)	107.56±0.29°
Longitude of the node (Ω)	151.44±0.12°
Periastron epoch (T)	1847.7±1.1
Argument of periastron (ω) (secondary)	318.4±1.1°
Details
40 Eridani A
Mass	0.78±0.08 M☉
Radius	0.804±0.006 R☉
Luminosity	0.4±0.01 L☉
Surface gravity (log g)	4.35±0.1 cgs
Temperature	5126±30 K
Metallicity	−0.36±0.02 dex
Rotation	~37–43 days
Rotational velocity (v sin i)	1.23 ± 0.28 km/s
Age	6.9±4.7 Gyr
40 Eridani B
Mass	0.573±0.018 M☉
Radius	0.01308±0.00020 R☉
Luminosity	0.01349±0.00054 L☉
Surface gravity (log g)	7.957±0.020 cgs
Temperature	17,200±110 K
40 Eridani C
Mass	0.222±0.22 M☉
Radius	0.274±0.011 R☉
Luminosity	0.00651±0.00013 L☉
Surface gravity (log g)	~5.5 cgs
Temperature	3,167±60 K
Age	1.8 Gyr
Other designations
ο Eri, 40 Eri, GJ 166, ADS 3093, CCDM J04153-0739
A: Keid, BD−07° 780, HD 26965, HIP 19849, HR 1325, SAO 131063, LHS 23, LTT 1907
B: BD−07° 781, HD 26976, SAO 131065, G 160-060, LHS 24, LTT 1908
C: DY Eri, BD−07°781 C, LHS 25, LTT 1909
Database references
SIMBAD	A
	B
	C

40 Eridani is a triple star system in the constellation of Eridanus, abbreviated 40 Eri. It has the Bayer designation Omicron Eridani, which is Latinized from ο Eridani and abbreviated Omicron Eri or ο Eri. Based on parallax measurements taken by the Gaia mission, it is about 16.3 light-years from the Sun.

The primary star of the system, designated 40 Eridani A and named Keid, is easily visible to the naked eye. It is orbited by a binary pair whose two components are designated 40 Eridani B and C, and which were discovered on January 31, 1783, by William Herschel. It was again observed by Friedrich Struve in 1825 and by Otto Struve in 1851.

In 1910, it was discovered that although component B was a faint star, it was white in color. This meant that it had to be a small star; in fact it was a white dwarf, the first discovered. Although it is neither the closest white dwarf, nor the brightest in the night sky, it is by far the easiest to observe; it is nearly three magnitudes brighter than Van Maanen's Star, the nearest solitary white dwarf, and unlike the companions of Procyon and Sirius it is not swamped in the glare of a much brighter primary.

Nomenclature

40 Eridani is the system's Flamsteed designation and ο² Eridani (Latinised to Omicron Eridani) its Bayer designation. The designations of the sub-components – 40 Eridani A, B and C – derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU). 40 Eridani C also bears the variable star designation DY Eridani.

The system bore the traditional name Keid derived from the Arabic word قيض (alqayḍ) meaning "the eggshells," alluding to its neighbour Beid (Arabic "egg"). In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems. It approved the name Keid for the component 40 Eridani A on 12 September 2016 and it is now so included in the List of IAU-approved Star Names.

Properties

40 Eridani A is a main-sequence dwarf of spectral type K1, 40 Eridani B is a 9th magnitude white dwarf of spectral type DA4, and 40 Eridani C is an 11th magnitude red dwarf flare star of spectral type M4.5e. When component B was a main-sequence star, it is thought to have been the most massive member of the system, but ejected most of its mass before it became a white dwarf. B and C orbit each other approximately 400 AU from the primary star, A. Their orbit has a semimajor axis of 35 AU and is rather elliptical with an orbital eccentricity of 0.410).

As seen from the 40 Eridani system, the Sun is a 3.4-magnitude star in Hercules, near the border with Serpens Caput.

Potential for life

The habitable zone of 40 Eridani A, where a planet could exist with liquid water, is near 0.68 AU from A. At this distance a planet would complete a revolution in 223 Earth days (according to the third of Kepler's laws) and 40 Eridani A would appear nearly 20% wider than the Sun does on Earth. An observer on a planet in the 40 Eridani A system would see the B-C pair as unusually bright white and reddish-orange stars in the night sky – magnitudes −8 and −6, slightly brighter than the appearance of Venus seen from Earth as the evening star.

It is unlikely that habitable planets exist around 40 Eridani B because they would have been sterilized by its evolution into a white dwarf. As for 40 Eridani C, it is prone to flares, which cause large momentary increases in the emission of X-rays as well as visible light. This would be lethal to Earth-type life on planets near the flare star.

Search for planets

40 Eridani A shows periodic radial velocity variations, which were suggested to be caused by a planetary companion. The 42-day period is close to the stellar rotation period, which made the possible planetary nature of the signal difficult to confirm. A 2018 study found that most evidence supports a planetary origin for the signal, but this has remained controversial, with a 2021 study characterizing the signal as a false positive. As of 2022, the cause of the radial velocity variations remained inconclusive.

Further studies in 2023 and 2024 concluded that the radial velocity signal very likely does originate from stellar activity, and not from a planet.

The candidate planet would have had a minimum mass of 8.47±0.47 M_🜨, and lie considerably interior to the habitable zone, receiving nine times more stellar flux than Earth, which is an even greater amount than Mercury, the innermost planet in the Solar System, on average receives from the Sun.

In fiction

In the Star Trek franchise, the planet Vulcan orbits 40 Eridani A. Vulcan has been referenced in relation to the real-life search for exoplanets in this system. The hypothetical planet 40 Eridani A b is also mentioned in the book Project Hail Mary as the home of the eponymous Eridian species.

Notes

1. From 40 Eridani the Sun would appear on the diametrically opposite side of the sky at the coordinates RA=16 15 16.32, Dec=07° 39′ 10.34″, which is located near the border of Hercules (constellation) and Serpens Caput, the closest bright star being Alpha Serpentis. The absolute magnitude of the Sun is 4.85, so, at a distance of 5.04 parsecs, the Sun would have an apparent magnitude ${\displaystyle {\begin{smallmatrix}m\ =\ M_{v}\ +\ 5\cdot ((\log _{10}\ 5.04)\ -\ 1)\ =\ 3.36\end{smallmatrix}}}$.
2. From ${\displaystyle \ h={\frac {\ a\ }{d}}\,,}$ where h is the apparent height, d is the distance of the object, and a is the actual size of the object.

References

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External links

• Keid at Jim Kaler's STARS.
• Omicron(2) Eridani entry at the Internet Stellar Database.

v t e Constellation of Eridanus
List of stars in Eridanus Eridanus in Chinese astronomy
Stars	Bayer α (Achernar) β (Cursa) γ (Zaurak) δ (Rana) ε (Ran) ζ (Zibal) η (Azha) θ (Acamar) θ ι κ λ μ ν ξ ο (Beid) ο (40, Keid) π ρ ρ ρ τ τ (Angetenar) τ τ τ τ τ τ τ υ υ (Theemin) υ (Beemim) υ φ χ ψ ω Flamsteed 14 15 17 (v) 39 (A) 45 51 (c) 53 (Sceptrum) 54 58 64 66 Variable DO DZ EF EK EM (d) EP KT HR 486 (p) 487 (p) 506 (q) 789 (s) 859 1008 (e) 1106 (y) 1143 (h) 1189 (f) 1190 (f) 1195 (g) 1483 1536 1614 HD 18742 (Ayeyarwady) 19467 28185 30562 30856 (Mouhoun) 30963 Other 2MASS J04151954−0935066 DENIS 0255−4700 Gliese 86 Gliese 180 GJ 1062 GJ 3293 GJ 3323 HIP 12961 (Koeia) LTT 1445 LP 890-9 Mothra WASP-22 (Tojil) WASP-35 WASP-50 (Chaophraya) WASP-78 WASP-79 (Montuno) WISE J0336−0143
Exoplanets 51 Eridani b ε Eridani b (AEgir) Gliese 86 b HD 10647 b HD 18742 b (Bagan) HD 28185 b HD 30562 b HD 30856 Ab (Nakanbé) WASP-79b (Pollera)
Nebulae	NGC 1535
Galaxies	NGC 782 852 939 1084 1132 1140 1154 1155 1157 1158 1164 1172 1187 1189 1190 1191 1192 1199 1222 1232 1234 1241 1253 1262 1266 1269 1291 1300 1309 1325 1332 1337 1345 1347 1353 1357 1369 1386 1395 1400 1403 1404 1407 1426 1427A 1436 1437 1439 1452 1460 1487 1531 1532 1592 1600 1614 1637 1721 1723 1725 1728 1741 Other Eridanus II ESO 198-13 ESO 0313-192 IC 1953 IC 2006 LEDA 74886 MRC 0406-244 PKS 0208-512 PKS 0405–385 PKS 0420-014 UGC 2812
Galaxy clusters Abell 383 Eridanus Cluster Eridanus Group MACS J0416.1-2403
Astronomical events GRB 080913 HE0435-1223
Category

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