A light curve for Lambda Eridani, plotted from TESS data[1]
Observation data Epoch J2000.0 Equinox J2000.0 (ICRS)
Constellation
Eridanus
Right ascension
05h 09m 08.78315s[2]
Declination
−08° 45′ 14.6908″[2]
Apparent magnitude (V)
4.27[3]
Characteristics
Spectral type
B2 IVne[4] or B2 III(e)p[5]
U−B color index
−0.90[3]
B−V color index
−0.19[3]
Variable type
λ Eri[6]
Astrometry
Radial velocity (Rv)
−2.51±5.43[7] km/s
Proper motion (μ)
RA: +0.25[2] mas/yr Dec.: −1.97[2] mas/yr
Parallax (π)
4.02 ± 0.18 mas[2]
Distance
810 ± 40 ly (250 ± 10 pc)
Absolute magnitude (MV)
−3.75[4]
Details
Mass
9,2[8]M☉
Radius
7.31[9]R☉
Luminosity
14,689[10]L☉
Surface gravity (log g)
4.32[11] cgs
Temperature
22,362[11] K
Metallicity [Fe/H]
−2.0[11] dex
Rotation
1.40346 d[4]
Rotational velocity (v sin i)
318[10] km/s
Age
21.0[8] Myr
Other designations
λ Eridani, 69 Eridani, CD−08°1040, FK5 190, HD 33328, HIP 23972, HR 1679, SAO 131824.[12]
Database references
SIMBAD
data
Lambda Eridani (λ Eri) is a star in the constellation Eridanus. It is visible to the naked eye on a dark night with an apparent visual magnitude of 4.27. The distance to this star, based upon an annual parallax shift of 0.00402 arcseconds, is roughly 810 light years.
λ Eri is classified in the General Catalogue of Variable Stars as a Beta Cephei variable.[13] The AAVSO International Variable Star Index defines a LERI type of variation. λ Eri is classified as LERI + GCAS since it shows both short term periodic variations and longer timescale eruptive variation.[6] It was one of the first stars where short-period variations were found.[4] The line profile variability periods are 0.702d and 0.269d, with intermittently present periods of 0.6d and 0.75d. The photometric amplitude of the variation is 0.010 magnitude.[5]
This is a giant or subgiant Be star with a stellar classification of B2 IVne[4] or B2 III(e)p,[5] depending on the source. It is spinning rapidly with a projected rotational velocity of 327 km/s.[7] Compare this to the estimated break-up velocity of 440 km/s.[14] This rotation is giving the star an oblate shape with an equatorial bulge that is 25% larger than the polar radius.[15] The most likely rotation period is deemed to be twice the period of variation, or 1.4 days.[4] The star also possesses a rotating circumstellar disc, seen edge on, which makes Lambda Eri a "shell star", where the disk appears more opaque than usual. [16]
Like most Be stars, Lambda Eridani emits soft X-rays. In 1993, a giant X-ray flare was observed in which the X-ray luminosity increased by a factor of six over a 39-hour period.[4] Lambda Eridani has about nine times the mass of the Sun, and seven times the Sun's radius. It radiates 14,700 times the solar luminosity from its outer atmosphere at an effective temperature of 22,362 K.
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LambdaEridani (λ Eri) is a star in the constellation Eridanus. It is visible to the naked eye on a dark night with an apparent visual magnitude of 4.27...
A LambdaEridani Variable is a class of Be stars that show small amplitude variations of a few hundredths of a magnitude. The variations are highly regular...
name of the star association consisting of this star along with LambdaEridani, Psi Eridani and Tau Orionis. According to a NASA catalogue of stars, Al Kursiyy...
HR 2501, also known as HD 49131 and HP Canis Majoris, is a star about 2,000 light years from the Earth, in the constellation Canis Major. It is a 5th magnitude...
Alpha Arae, Latinized from α Arae, is the second brightest star in the southern constellation of Ara. With an average apparent visual magnitude 2.93, it...
of these are thought to be pulsating stars and are sometimes called LambdaEridani variables. Porter, John M.; Rivinius, Thomas (2003). "Classical Be Stars"...
Chi Ophiuchi, Latinized from χ Ophiuchi, is a variable star in the equatorial constellation of Ophiuchus. It has a blue-white hue and is faintly visible...
an effective temperature of 15,212 K in its outer envelope. It is a λ Eridani variable, or periodic Be star, with a pulsation cycle lasting 1.073 days...
Index lists Eta Centauri as both a Gamma Cassiopeiae variable and a LambdaEridani variable with variations caused by its rotation and pulsations. Eta...
43 - 4.46. The International Variable Star Index classifies it as a LambdaEridani variable. The correct Bayer designation for ο Puppis has been debated...
Kappa Ursae Majoris Binary star system 3.559 Lambda Geminorum Triple star system 3.56 Upsilon4 Eridani Binary star system 3.56 Delta Pavonis Star 3.56...
binary system of the white dwarf 40 Eridani B and the main sequence red dwarf 40 Eridani C. The pair 40 Eridani B/C was discovered by William Herschel...
currently thought more likely to be a different type of variable, possibly a λ Eridani variable or rotating ellipsoidal variable. This object is a B-type main-sequence...
done by Popper in 1954, measuring a 21 km/s gravitational redshift of 40 Eridani B. The redshift of Sirius B was finally measured by Greenstein et al. in...
absolutno by Karel Čapek. /ˈapsolutno/ Eridanus θ1 Eridani A Acamar /ˈækəmɑːr/ Eridanus α Eridani A Achernar The name was originally Arabic: آخر النهر...
Sebastian; Paulson, Diane B. (November 2006), "The extrasolar planet e Eridani b – orbit and mass", The Astronomical Journal, 132 (5): 2206–2218, arXiv:astro-ph/0610247...
Stellar black hole Compact star Quark star Exotic star Stellar core: EF Eridani Failed and theoretical stars Substellar object Brown dwarf Sub-brown dwarf...
nearest M-type red giant, and the 25th brightest star in the night sky. Beta Eridani (Cursa) 90±0.9 A3 III var or A3 IV 2.4 2 2.796 Kappa Ophiuchi 91.5±0.5...