14 Lacertae

14 Lacertae

A visual band light curve for V360 Lacertae, adapted from Linnell et al. (2006)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Lacerta
Right ascension 22h 50m 21.77721s[2]
Declination +41° 57′ 12.1795″[2]
Apparent magnitude (V) 5.91[1]
Characteristics
Spectral type B3IV:eaV[3] (B4 + F9 III)[4]
U−B color index −0.508[1]
B−V color index +0.083[1]
Variable type β Lyr[3]
Astrometry
Radial velocity (Rv)−15.8±3.1[5] km/s
Proper motion (μ) RA: +6.047[2] mas/yr
Dec.: +1.124[2] mas/yr
Parallax (π)2.0147 ± 0.1990 mas[2]
Distance1,600 ± 200 ly
(500 ± 50 pc)
Orbit[6]
Period (P)10.085415±0.000080 d
Eccentricity (e)0.0
Periastron epoch (T)2441170.285±0.029
Semi-amplitude (K1)
(primary)		25.8±1.7 km/s
Semi-amplitude (K2)
(secondary)		159.2±0.2 km/s
Details[1]
14 Lac A
Mass7.45±0.3 M☉
Radius(polar) 7.55 R☉
Surface gravity (log g)3.55 cgs
Temperature(Polar) 18,000±1,000 K
14 Lac B
Mass1.21±0.05 M☉
Radius(polar) 8.85 R☉
Surface gravity (log g)2.65 cgs
Temperature(polar) 6,000±200 K
Other designations
14 Lac, V360 Lac, BD+41° 4623, HD 216200, HIP 112778, HR 8690, SAO 52412, WDS J22504+4157[7]
Database references
SIMBADdata

14 Lacertae is a binary star[1] system in the northern constellation Lacerta, located around 1,600 light years away.[2] It has the variable star designation V360 Lacertae;[7] 14 Lacertae is the Flamsteed designation. The system is barely visible to the naked eye in good seeing conditions, having a peak apparent visual magnitude of 5.91.[8] It is moving closer to the Earth with a heliocentric radial velocity of −16 km/s.[5]

This is a double-lined spectroscopic binary in a close, circular orbit with a period of 10.08 days and a separation of 40.327 R☉ (28.055 Gm). The orbital inclination is 65°±1°. 14 Lac is a variable star system that, once per orbit, shows a primary minimum with a 0.07 magnitude decrease and a secondary minimum with a decrease of 0.02. The primary component is a Be star that is spinning rapidly at its critical velocity. The lower mass secondary is synchronously rotating and is filling its Roche lobe. The rapid rotation of the primary may have been caused by mass transfer from the secondary.[1]

Samus et al. (2017) classify this as a detached Beta Lyrae-type eclipsing binary, although they note there is some uncertainty in the classification.[3] Bossi et al. (1998) argued that the system is neither an eclipsing binary nor an ellipsoidal variable. Instead they propose the variability is caused by distortion of a gaseous shell by the secondary component.[9] Linnell et al. (2006) demonstrated that the light curve is mostly caused by tidal distortion in combination with illumination of the lower mass secondary by the primary.[1]

  1. ^ a b c d e f g h Cite error: The named reference Linnell2006 was invoked but never defined (see the help page).
  2. ^ a b c d e f Cite error: The named reference gaia_dr2 was invoked but never defined (see the help page).
  3. ^ a b c Cite error: The named reference Samus2017 was invoked but never defined (see the help page).
  4. ^ Cite error: The named reference Harmanec2015 was invoked but never defined (see the help page).
  5. ^ a b Cite error: The named reference Gontcharov2006 was invoked but never defined (see the help page).
  6. ^ Cite error: The named reference Hill1997 was invoked but never defined (see the help page).
  7. ^ a b Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  8. ^ Cite error: The named reference Malkov2006 was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Bossi1998 was invoked but never defined (see the help page).