NGTS-6

Last updated
NGTS-6
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Caelum [1]
Right ascension 05h 03m 10.90284s [2]
Declination −30° 23′ 57.7189″ [2]
Apparent magnitude  (V)14.12±0.03 [3]
Characteristics
Evolutionary stage main sequence [2]
Spectral type K [4]
Astrometry
Radial velocity (Rv)−19.14±0.01 [4] km/s
Proper motion (μ)RA: −9.308 mas/yr [2]
Dec.: −22.014 mas/yr [2]
Parallax (π)3.2536±0.0126  mas [2]
Distance 1,002 ± 4  ly
(307 ± 1  pc)
Details [4]
Mass 0.767±0.025  M☉
Radius 0.754±0.013  R☉
Luminosity 0.256±0.009  L☉
Surface gravity (log g)4.7+1.1
−0.7  cgs
Temperature 4,730+44
−40  K
Metallicity [Fe/H]0.11±0.09  dex
Rotational velocity (v sin i)2.85±0.43 km/s
Age 9.77+0.25
−0.54  Gyr
Other designations
NGTS-6, TOI-448, TIC 1528696, 2MASS J05031090-3023576
Database references
SIMBAD data
Exoplanet Archive data

NGTS-6 is a star located in the southern constellation Caelum, the chisel. It has an apparent magnitude of 14.12, [3] making it readily visible in telescopes with an aperture of at least 203 millimeters; it can also be viewed in telescopes with an aperture between 152 and 203 mm, albeit faintly. The star is located relatively far at a distance of 1,002 light years based on parallax measurements from the Gaia spacecraft, [2] but it is drifting closer with a heliocentric radial velocity of −19.14  km/s . [4]

NGTS-6 is a K-type main sequence star that has 76.7% the mass of the Sun and 75.4% of the Sun's radius. [4] However, it only radiates 25.6% of the Sun's luminosity [4] from its photosphere at an effective temperature of 4,730  K , [4] giving it an orange hue when viewed in a telescope. It is metal enriched with of the Sun's abundance of iron. [4] Such stars are more likely to form giant planets. NGTS-6 is estimated to be 9.77 billion years old and it spins modestly with a projected rotational velocity of 2.85  km/s . [4]

Planetary system

NGTS-6b compared to Jupiter NGTS-6b comparision.png
NGTS-6b compared to Jupiter

In 2018, a ultra-hot Jupiter was discovered orbiting the star based on transit data from the Next Generation Transit Survey. It was confirmed a year later based on doppler spectroscopy data from CORALIE and FEROS. NGTS-6b orbits extremely closely to its host star within a 21.17 hour period, making it an ultra-short period planet. The planet is 33.9% more massive than Jupiter, but it is 32.6% larger as a result of tidal heating from its close proximity. [4] The system was included in a 2024 survey as a potential target for studying the orbital decay of exoplanets. [5]

The NGTS-6 planetary system [4]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(hours)		 Eccentricity Inclination Radius
NGTS-6b1.339±0.028  MJ 0.01677±0.0003221.169404±0.000007920.00 (fixed)78.231+0.262
−0.210 ° 		1.326+0.097
−0.112  RJ

References

  1. ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific . 99 (617): 695. Bibcode:1987PASP...99..695R. doi: 10.1086/132034 . Constellation record for this object at VizieR.
  2. 1 2 3 4 5 6 7 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  3. 1 2 Zacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.; Bartlett, J. L.; Monet, D. G.; Zacharias, M. I. (January 14, 2013). "The Fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)". The Astronomical Journal. 145 (2): 44. arXiv: 1212.6182 . Bibcode:2013AJ....145...44Z. doi: 10.1088/0004-6256/145/2/44 . ISSN   0004-6256. S2CID   119299381.
  4. 1 2 3 4 5 6 7 8 9 10 11 Vines, Jose I; et al. (November 2019). "NGTS-6b: an ultrashort period hot-Jupiter orbiting an old K dwarf". Monthly Notices of the Royal Astronomical Society. 489 (3): 4125–4134. arXiv: 1904.07997 . Bibcode:2019MNRAS.489.4125V. doi: 10.1093/mnras/stz2349 . ISSN   0035-8711. S2CID   202542422.
  5. ↑ Weinberg, Nevin N.; Davachi, Niyousha; Essick, Reed; Yu, Hang; Arras, Phil; Belland, Brent (January 2024). "Orbital Decay of Hot Jupiters due to Weakly Nonlinear Tidal Dissipation". The Astrophysical Journal. 960 (1): 50. arXiv: 2305.11974 . Bibcode:2024ApJ...960...50W. doi: 10.3847/1538-4357/ad05c9 . ISSN   0004-637X. S2CID   258832490.
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