FL Lyrae

FL Lyrae

A light curve for FL Lyrae, plotted from TESS data[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Lyra
Right ascension 19h 12m 04.862s[2]
Declination +46° 19′ 26.87″[2]
Apparent magnitude (V) 9.36[3]
Characteristics
Spectral type G0V[4] (F8 + G8)[5]
B−V color index +0.55[3]
Variable type Algol[6]
Astrometry
Radial velocity (Rv)−39.20[7] km/s
Proper motion (μ) RA: −0.172 mas/yr[2]
Dec.: +46.008 mas/yr[2]
Parallax (π)7.4577 ± 0.0122 mas[2]
Distance437.3 ± 0.7 ly
(134.1 ± 0.2 pc)
Absolute magnitude (MV)3.84±0.08
5.30±0.16[4]
Details
FL Lyr A
Mass1.218±0.016[4] M☉
Radius1.283±0.030[4] R☉
Luminosity2.17[4] L☉
Surface gravity (log g)4.31±0.02[4] cgs
Temperature6,363±353[8] K
Metallicity [Fe/H]−0.34[6] dex
Rotational velocity (v sin i)29.2[6] km/s
Age2.29[5] Gyr
FL Lyr B
Mass0.958±0.011[4] M☉
Radius0.963±0.030[4] R☉
Luminosity0.65[4] L☉
Surface gravity (log g)4.45±0.03[4] cgs
Temperature5,239±541[8] K
Other designations
FL Lyr, BD+46° 2641, HD 179890, HIP 94335, SAO 48190, KIC 9641031[9]
Database references
SIMBADdata

FL Lyrae is the variable star designation for an eclipsing binary star system in the northern constellation of Lyra. The combined apparent magnitude of the pair is 9.36,[3] which means they are too faint to be seen with the naked eye. Parallax measurements put the system at a distance of around 437 light years from the Sun. This star system was in the view field of the Kepler space telescope during 2009−2014,[5] which allowed monitoring during that spacecraft's mission.[8]

The variability of this system was discovered from photographic plates in 1935.[5] It is a binary star system with an orbital plane that is nearly aligned with the line of sight to the Earth. Once every 2.1781542 day orbit, each of the closely orbiting stars eclipses its partner, causing a net magnitude drop to 9.4 during the primary eclipse and to magnitude 9.1 when the secondary component is eclipsed. The secondary member covers 51% of the larger star during the primary eclipse, while the primary covers 88% of the secondary.[4]

The measureable properties of an eclipsing binary can allow the physical parameters of the individual components to be worked out in some detail. The primary component has 122% of the Sun's mass, spans 128% of the radius of the Sun, and is emitting 217% of the Sun's luminosity. It is most likely an F-type main sequence star with a stellar classification of F8.[5] The secondary is smaller, with 96% of the mass of the Sun, 96% of the Sun's radius, and radiates just 65% of the Sun's luminosity.[4] This is a G-type main sequence star of class G8.[5]

Based upon light variations measured during eclipses by the Kepler spacecraft, the system may contain a third body with twice the mass of Jupiter and an orbital period of under seven years. As of 2015, this remains to be confirmed.[5]

  1. ^ Cite error: The named reference MAST was invoked but never defined (see the help page).
  2. ^ a b c d Cite error: The named reference GaiaEDR3 was invoked but never defined (see the help page).
  3. ^ a b c Cite error: The named reference tycho2 was invoked but never defined (see the help page).
  4. ^ a b c d e f g h i j k l Cite error: The named reference rasm79_2_131 was invoked but never defined (see the help page).
  5. ^ a b c d e f g Cite error: The named reference arxiv20151007 was invoked but never defined (see the help page).
  6. ^ a b c Cite error: The named reference aa504_3_829 was invoked but never defined (see the help page).
  7. ^ Cite error: The named reference al32_11_759 was invoked but never defined (see the help page).
  8. ^ a b c Cite error: The named reference mnras437_4_3473 was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).