NGTS-6
| Observation data Epoch J2000.0 Equinox 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
[edit]
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]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (hours) |
Eccentricity | Inclination (°) |
Radius |
|---|---|---|---|---|---|---|
| NGTS-6b | 1.339±0.028 MJ | 0.01677±0.00032 | 21.169404±0.00000792 | 0.00 (fixed) | 78.231+0.262 −0.210 |
1.326+0.097 −0.112 RJ |
References
[edit]- ↑ 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.
- 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.
- 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.
- 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.
- ↑ 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.
