5 Vulpeculae

5 Vulpeculae
Map of the constellation Vulpecula
5 Vul in the constellation Vulpecula (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Vulpecula
Right ascension 19h 26m 13.2463s[1]
Declination +20° 05′ 51.8394″[1]
Apparent magnitude (V) 5.65±0.010[2]
Characteristics
Spectral type A0 V[3]
Apparent magnitude (U) 5.62±0.012[2]
Apparent magnitude (B) 5.66±0.011[2]
Astrometry
Radial velocity (Rv)−20.9±2.9[4] km/s
Proper motion (μ) RA: +3.395±0.114[1] mas/yr
Dec.: −34.787±0.137[1] mas/yr
Parallax (π)13.8921 ± 0.0900 mas[1]
Distance235 ± 2 ly
(72.0 ± 0.5 pc)
Absolute magnitude (MV)1.29[5]
Details[3]
Mass2.33±0.02 M☉
Radius2.7[6] R☉
Luminosity34±2 L☉
Surface gravity (log g)4.0[7] cgs
Temperature9,840+91
−90 K
Rotational velocity (v sin i)154 km/s
Age198[7] Myr
Other designations
5 Vul, BD+19° 4015, HD 182919, HIP 95560, HR 7390, SAO 104831[8]
Database references
SIMBADdata

5 Vulpeculae is a single,[9] white-hued star in the northern constellation of Vulpecula.[8] It is situated amidst a random concentration of bright stars designated Collinder 399,[10] or Brocchi's Cluster. This is a faint star that is just visible to the naked eye with an apparent visual magnitude of 5.60.[4] Based upon an annual parallax shift of 13.8921±0.0900 mas,[1] it is located around 235 light years from the Sun. It is moving closer with a heliocentric radial velocity of −21 km/s,[4] and will make its closest approach in 2.5 million years at a separation of around 120 ly (36.89 pc).[5]

This is a young A-type main-sequence star with a stellar classification of A0 V.[3] It is a rapidly rotating star[11] with a projected rotational velocity of 154 km/s.[3] The star has an estimated 2.33[3] times the mass of the Sun and about 2.7[6] times the Sun's radius. It is radiating 34 times the Sun's luminosity from its photosphere at an effective temperature of 8,940 K.[3]

A warm debris disk was detected by the Spitzer Space Telescope at a temperature of 206 K (−89 °F; −67 °C), orbiting 13 Astronomical units from the host star.[12] Although this finding has not been directly detected, the emission signature indicates the disk is in the form of a thin ring. The emission displays weak transient absorption features that are indicative of kilometer-sized exocomets that are undergoing evaporation as they approach the host star.[11] These absorption features have been observed to vary on time scales of hours, days, or months.[13]

  1. ^ a b c d e f Cite error: The named reference Gaia DR2 was invoked but never defined (see the help page).
  2. ^ a b c Cite error: The named reference Harmanec2020 was invoked but never defined (see the help page).
  3. ^ a b c d e f Cite error: The named reference zorec2012 was invoked but never defined (see the help page).
  4. ^ a b c Cite error: The named reference Gontcharov2006 was invoked but never defined (see the help page).
  5. ^ a b Cite error: The named reference Anderson2012 was invoked but never defined (see the help page).
  6. ^ a b Cite error: The named reference cadars was invoked but never defined (see the help page).
  7. ^ a b Cite error: The named reference Chen2014 was invoked but never defined (see the help page).
  8. ^ a b Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Eggleton2008 was invoked but never defined (see the help page).
  10. ^ Cite error: The named reference Baumgardt1998 was invoked but never defined (see the help page).
  11. ^ a b Cite error: The named reference Montgomery2012 was invoked but never defined (see the help page).
  12. ^ Cite error: The named reference Morales2009 was invoked but never defined (see the help page).
  13. ^ Cite error: The named reference Montgomery2014 was invoked but never defined (see the help page).