| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Gemini[note 1] |
| Right ascension | 07h 49m 55.05s[1] |
| Declination | 27° 21′ 47.45″[1] |
| Apparent magnitude (V) | 6.92[2] |
| Characteristics | |
| Evolutionary stage | Main sequence[3] |
| Spectral type | G5V[3] |
| Variable type | BY Draconis[4][5] |
| Astrometry | |
| Radial velocity (Rv) | −16.07±0.13[2] km/s |
| Proper motion (μ) | RA: −10.0268±0.0846 mas/yr[2] Dec.: −11.3143±0.0487 mas/yr[2] |
| Parallax (π) | 44.6848 mas[6] |
| Distance | 73.035±0.073 ly (22.4035±0.0225 pc)[2] |
| Absolute magnitude (MV) | 5.19[7] |
| Details[8] | |
| Mass | 0.99±0.03 M☉ |
| Radius | 0.912±0.034 R☉ |
| Luminosity | 0.753±0.026 L☉ |
| Surface gravity (log g) | 4.52±0.05[3] cgs |
| Temperature | 5640±74 K |
| Metallicity [Fe/H] | 0.03±0.05[3] dex |
| Rotation | 6.45±0.05 d |
| Rotational velocity (v sin i) | 7.3±0.3 km/s |
| Age | 414±23 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 63433 (TOI-1726, V377 Geminorum) is a G-type main sequence star located 73 light-years from Earth in the zodiacal constellation Gemini,[8][note 1] visually close to the star Pollux.[6] It is classified as a Sun-like star, having a mass 99% similar and a size 91% similar to that of the Sun.[8] However, it is a much younger star, less than one tenth as old with an age of about 400 million years.[8][a] With an apparent magnitude of 6.9, it is not visible to the naked eye, but can be seen with a small telescope.[11] Based on its kinematic, rotational and lithium abundance properties, it is part of the Ursa Major Moving Group.[8] There are three exoplanets orbiting it, one is classified as an Earth-sized planet, while the two others are mini-Neptunes.[3]
Characteristics
HD 63433 is a Sun-like star, having a radius of 0.912 R☉, a mass of 0.99 M☉, an effective temperature of 5640 K and a spectral type G5V.[8] Its properties are quite similar to those of the Sun, which has a spectral type G2V and a temperature of 5772 K.[12] HD 63433, however, is much younger than the Sun, having an age of 414 million years,[8] just 9% of the solar age of 4.6 billion years.[10]
It is also a variable star, belonging to the class of BY Draconis variables,[4][5] stars which have variations in their luminosity due to their rotation together with sunspots and other chromospheric activities. The brightness of the star varies by 0.05 magnitudes over a period of 6.46 days.[5] It has the variable-star designation V377 Geminorum.[6][5]
With an apparent magnitude of 6.92m,[2] it is below the limit for naked-eye visibility, generally defined as 6.5m,[13] which would mean that this star is not visible to the naked eye, but easily visible using a small telescope[11] or binoculars.[14] Despite being faint, HD 63433 is actually the third-brightest star with transiting exoplanets confirmed by the Transiting Exoplanet Survey Satellite, with only Pi Mensae (5.65m)[15] and HR 858 (6.38m)[16] being brighter.[8][17]
According to stellar kinematics, lithium abundance and stellar rotation, HD 63433 is part of the Ursa Major moving group.[8] It was initially identified as a possible member of this group by Gaidos (1998)[18] and included as a possible member in later analyses, until HD 63433's membership in this moving group was finally confirmed by Mann et al. in 2020.[8] As it is part of this moving group, its age is estimated at 414 ± 23 million years, the same as the group.[8]
It is located in the northern hemisphere, about 73 light-years from the Earth, in the constellation of Gemini.[11] It is visually close to Pollux, the brightest star in the constellation.[6] HD 63433 is predicted to approach within 7.33 light-years of the Sun in 1.33 million years.[19] That will make it one of the nearest stars to the Sun. Its closest neighbor is the orange dwarf HD 63991, located at a distance of 2.7 light years.[11]
| Name | Distance
(light-years) |
|---|---|
| HD 63991 | 2.7 |
| LSPM J0801+2342 | 6.1 |
| HD 68017 | 9 |
| BD+31 1781 | 9.1 |
| G 90-52 | 9.2 |
Planetary system
The star HD 63433 is orbited by 3 exoplanets, all discovered by the transit method.
The first ones to be discovered, HD 63433 b and HD 63433 c, are mini-Neptunes[20] that were discovered in by Mann et al. in 2020 using the Transiting Exoplanet Survey Satellite.[21] In 2024, an additional planet was discovered, after an analysis of a transit signal detected by TESS. Named HD 63433 d, it is an Earth-sized planet.[22]
According to theoretical models, the compositions of the mini-Neptunes HD 63433 b and c are mostly silicate and water, with no iron dominance, surrounded by a gaseous envelope which, in the case of planet c, makes up around 2% of the planet.[20]
The planetary system of HD 63433 is quite young, at around 400 million years old, it is only 9.13% as old as the Solar System.[3][22][b] HD 63433 d is also the smallest planet that is less than 500 million years old.
| Temperature comparisons |
HD 63433 b[20] | HD 63433 c[20] | HD 63433 d[3] |
| Global equilibrium temperature | 769 – 967 K 496 – 694 °C 925 – 1281 °F |
540 – 679 K 267 – 406 °C 513 – 763 °F |
1040 K 767 °C 1413 °F |
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| d | — | 0.0503±0.0027 | 4.21 | 0.16+0.36 −0.12 |
88.73±1° | 1.073+0.046 −0.044 R🜨 |
| b | <21.76 M🜨 | 0.0719+0.0044 −0.0031 |
7.11 | 0.24+0.27 −0.18 |
— | 2.14+0.087 −0.069 R🜨 |
| c | 15.54±3.86 M🜨 | 0.1458±0.015 | 20.55 | 0.161+0.014 −0.013 |
— | 2.692+0.108 −0.088 R🜨 |
HD 63433 b
The middle planet, HD 63433 b, is a mini-Neptune planet that was discovered together with HD 63433 c.[3] HD 63433 b is 2.14 times larger than Earth,[20] but is about 45% smaller than Neptune.[c] The planet has an upper mass limit of 21.7 M🜨,[20] which is 21% greater than the mass of Neptune (17.15 M🜨 [23]). These values calculate an upper density limit of 13 g/cm3,[20] 2 times greater than that of Earth,[note 2] and similar to that of the chemical element Mercury. HD 63433 b orbits its parent star at a distance of 0.0719 astronomical units (10,760,000 km) – about 5 times closer than Mercury is to the Sun – and completes one revolution every 7 days and 3 hours. The relative proximity of its star makes it hot, with an equilibrium temperature between 769 and 967 Kelvin (496 and 694 °C).[20][d]
HD 63433 b was probably a mini-Neptune that later lost its atmosphere.[25] Some factors, such as the fact that no absorption of Ly-α was detected during its transit, and its mass-loss timescale being shorter than the age of the planetary system, indicate that it has already lost its primordial atmosphere, and could be a rocky planetary core.[25] However, if HD 63433 b were a rocky core, it would need to be unusually massive and, therefore, a water-rich composition in addition to an atmosphere with a high mean molecular weight could explain both the radius and the non-detection of the Lyα.[25]
HD 63433 c
The outermost planet, HD 63433 c, is a mini-Neptune planet discovered together with HD 63433 b.[8] It is 2.7 times larger than Earth,[20] but 30% smaller than the Solar System's ice giants, Neptune and Uranus. Being 15.5 times more massive than the Earth,[20] it is more massive than Uranus (14.54 M🜨), but still less massive than Neptune (17.15 M🜨). The density of HD 63433 c calculated at 4.6 g/cm3, slightly lower than that of Earth,[20] but greater than the densities of all gas giants in the Solar System.
Orbiting its star at a distance of 0.145 astronomical units (21,700,000 km) in a orbital period of 20 days,[20] it is the outermost planet in its planetary system, but still close to its star, making it a warm planet, with a planetary equilibrium temperature estimated between 267 and 406 °C.[20][e]
Due to the high radiation received from its star, the atmosphere of HD 63433 c, made up of hydrogen, is slowly being stripped away and escaping from the planet, like a hot air balloon.[26] The hot gas escapes into the space at a velocity of 50 km/s, forming a gas cocoon 12 times larger than the planet itself.[26] As its atmosphere evaporates, HD 63433 c will slowly become a super-Earth planet.[26]
HD 63433 d
HD 63433 d was the last planet to be discovered in the system, 4 years after planets b and c.[3] With a diameter of ~13,690 km, it is very similar to Earth in size, being only 7% larger, but its mass is currently unknown.[3] It is the innermost planet orbiting HD 63433, having a semi-major axis (mean distance from its star) of 0.0503 astronomical units (7,520,000 km) and an orbital period of just 4 days.[3] The extreme proximity to its star makes it extremely hot, having a daytime temperature estimated at 1,260 °C (2,300 °F),[3] [f] hot enough to melt all the minerals present on its surface,[27] as well as being tidally locked, meaning that one half of the planet is always facing towards its star, while the other is always facing away from it.[28][22] The planet also possibly lacks a substantial atmosphere.[3][22][27]
It is believed that the dayside of the planet, always facing its star due to tidal locking, is fully composed of lava due to the high surface temperature,[29][22] in addition to possibly having volcanic activity.[30][31] Meanwhile, the nightside of the planet, which never faces its star, may be the opposite, resembling Pluto with glaciers of frozen nitrogen.[32]
HD 63433 d was discovered in 2024, through an analysis of a transit observation made by the Transiting Exoplanet Survey Satellite (TESS).[22] As two other planets had already been discovered in the system, the transit signals of these objects were removed, thus revealing an additional transit signal that reappeared every 4.2 days.[22][33][3] Further investigation allowed researchers to confirm that this signal was from another orbiting exoplanet, now called HD 63433 d.[22] The discovery was announced on January 10, 2024, in The Astronomical Journal.[28][32]
Scientific importance
The HD 63433 planetary system plays an important role in understanding the evolution of planetary systems in the first billion years after formation.[8][3] As HD 63433 is relatively bright (6.9m) and close (73 ly away), its planets b and c can have their atmospheres characterized by the Hubble Space Telescope and James Webb Space Telescope.[25] This star is also a favorable target for studies of atmospheric mass loss in exoplanets, as it is a young and active star with close-in mini-Neptune planets, in addition to having a negative radial velocity (−16.07 km/s).[25]
See also
- Ursa Major moving group
- Exoplanet
- Transiting Exoplanet Survey Satellite
- Mini-Neptune
- Lava planet
- List of star systems within 70–75 light-years
Notes and references
- ^ a b 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.
- ^ a b c d e "HD 63433 | NASA Exoplanet Archive". exoplanetarchive.ipac.caltech.edu. Retrieved 2024-01-13.
- ^ a b c d e f g h i j k l m n o p Capistrant, Benjamin K.; Soares-Furtado, Melinda; Vanderburg, Andrew; Jankowski, Alyssa; Mann, Andrew W.; Ross, Gabrielle; Srdoc, Gregor; Hinkel, Natalie R.; Becker, Juliette (2024-01-09), "TESS Hunt for Young and Maturing Exoplanets (THYME) XI: An Earth-sized Planet Orbiting a Nearby, Solar-like Host in the 400Myr Ursa Major Moving Group", The Astronomical Journal, 167 (2): 54, arXiv:2401.04785, Bibcode:2024AJ....167...54C, doi:10.3847/1538-3881/ad1039
- ^ a b Notsu, Yuta; Honda, Satoshi; Maehara, Hiroyuki; Notsu, Shota; Namekata, Kosuke; Nogami, Daisaku; Shibata, Kazunari (2017-02-01). "Spectroscopic observations of active solar-analog stars having high X-ray luminosity, as a proxy of superflare stars". Publications of the Astronomical Society of Japan. 69 (1): 12. arXiv:1611.03659. doi:10.1093/pasj/psw116. ISSN 0004-6264.
- ^ a b c d "VSX : Detail for V0377 Gem". www.aavso.org. Retrieved 2024-01-21.
- ^ a b c d e "HD 63433". simbad.cds.unistra.fr. Retrieved 2024-01-11.
- ^ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
- ^ a b c d e f g h i j k l m Mann, Andrew W.; Johnson, Marshall C.; Vanderburg, Andrew; Kraus, Adam L.; Rizzuto, Aaron C.; Wood, Mackenna L.; Bush, Jonathan L.; Rockcliffe, Keighley; Newton, Elisabeth R.; Latham, David W.; Mamajek, Eric E.; Zhou, George; Quinn, Samuel N.; Thao, Pa Chia; Benatti, Serena (2020-09-24). "TESS Hunt for Young and Maturing Exoplanets (THYME). III. A Two-planet System in the 400 Myr Ursa Major Group". The Astronomical Journal. 160 (4): 179. arXiv:2005.00047. Bibcode:2020AJ....160..179M. doi:10.3847/1538-3881/abae64. ISSN 0004-6256.
- ^ "HD 63433". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2024-01-23.
- ^ a b Bonanno, A.; Schlattl, H.; Paterno`, L. (August 2002). "The age of the Sun and the relativistic corrections in the EOS". Astronomy & Astrophysics. 390 (3): 1115–1118. arXiv:astro-ph/0204331. Bibcode:2002A&A...390.1115B. doi:10.1051/0004-6361:20020749. ISSN 0004-6361.
- ^ a b c d e "★ HD 63433". Stellar Catalog. Retrieved 2024-01-11.
- ^ "Sun Fact Sheet". nssdc.gsfc.nasa.gov. Retrieved 2024-01-11.
- ^ Curtis, Heber Doust (1903-01-01). "On the limits of unaided vision". Lick Observatory Bulletin. 38: 67–69. Bibcode:1903LicOB...2...67C. doi:10.5479/ADS/bib/1903LicOB.2.67C. ISSN 0075-9317. S2CID 124815809.
- ^ Siegel-Itzkovich, Judy (January 14, 2024). "Earth-sized exoplanet discovered in 'our solar backyard' by international team". The Jerusalem Post. Archived from the original on January 20, 2024. Retrieved January 20, 2024.
- ^ Johnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966-01-01). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99–110. Bibcode:1966CoLPL...4...99J.
- ^ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000-03-01). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN 0004-6361.
- ^ "NASA Exoplanet Space Institute". exoplanetarchive.ipac.caltech.edu. Retrieved January 15, 2024.
- ^ Gaidos, Eric J. (November 1998). "Nearby Young Solar Analogs. I. Catalog and Stellar Characteristics". Publications of the Astronomical Society of the Pacific. 110 (753): 1259–1276. Bibcode:1998PASP..110.1259G. doi:10.1086/316251. ISSN 0004-6280.
- ^ Bailer-Jones, C.A.L.; et al. (2018), "New stellar encounters discovered in the second Gaia data release", Astronomy & Astrophysics, 616: A37, arXiv:1805.07581, Bibcode:2018A&A...616A..37B, doi:10.1051/0004-6361/201833456, S2CID 56269929.
- ^ a b c d e f g h i j k l m n Mallorquín, M.; Béjar, V. J. S.; Lodieu, N.; Osorio, M. R. Zapatero; Tabernero, H.; Mascareño, A. Suárez; Zechmeister, M.; Luque, R.; Pallé, E.; Montes, D. (2023-03-01). "Dynamical masses of two young transiting sub-Neptunes orbiting HD 63433". Astronomy & Astrophysics. 671: A163. arXiv:2303.15411. Bibcode:2023A&A...671A.163M. doi:10.1051/0004-6361/202245397. ISSN 0004-6361.
- ^ "HD 63433". Open Exoplanet Catalogue. Archived from the original on January 14, 2024. Retrieved January 14, 2024.
- ^ a b c d e f g h Gohd, Chelsea (January 11, 2024). "Discovery Alert: Earth-sized Planet Has a 'Lava Hemisphere'". science.nasa.gov. Retrieved January 10, 2024.
- ^ a b "Neptune Fact Sheet". nssdc.gsfc.nasa.gov. Retrieved January 24, 2024.
- ^ "Facts About Earth - NASA Science". science.nasa.gov. Retrieved 2023-12-04.
- ^ a b c d e Zhang, Michael; Knutson, Heather A.; Wang, Lile; Dai, Fei; Santos, Leonardo A. dos; Fossati, Luca; Henry, Gregory W.; Ehrenreich, David; Alibert, Yann; Hoyer, Sergio; Wilson, Thomas G.; Bonfanti, Andrea (January 2022). "Detection of Ongoing Mass Loss from HD 63433c, a Young Mini-Neptune". The Astronomical Journal. 163 (2): 68. arXiv:2106.05273. Bibcode:2022AJ....163...68Z. doi:10.3847/1538-3881/ac3f3b. ISSN 1538-3881.
- ^ a b c "Puffy Planets Lose Atmospheres, Become Super-Earths". hubblesite.org. February 3, 2022. Retrieved January 19, 2024.
- ^ a b Thomson, Jess (January 12, 2024). "Hellish World With 2,294 F 'Lava Hemisphere' Discovered by NASA". Newsweek. Retrieved January 23, 2024.
- ^ a b Robert, Lea (January 12, 2024). "Newfound Earth-size exoplanet has a scorching-hot lava side". Space. Archived from the original on January 12, 2024. Retrieved January 12, 2024.
- ^ Gough, Evan (January 12, 2024). "Half of this Exoplanet is Covered in Lava". Universe Today.
- ^ Staff, Buzz (16 January 2024). "NASA Telescope Discovers Half-Lava Exoplanet Of Same Size As Earth". News18. Retrieved January 16, 2024.
- ^ Whitwam, Ryan (January 15, 2024). "Astronomers Discover Earth-Sized Planet That's Half Lava". ExtremeTech. Retrieved January 17, 2024.
- ^ a b Szondy, David (January 11, 2024). "Tidally locked exo-Earth has a lava ocean hemisphere". New Atlas. Archived from the original on January 16, 2024. Retrieved January 14, 2024.
- ^ "'Extra hot and young' Earth-sized exoplanet with a 'lava hemisphere' discovered". wionews.com. January 17, 2024.
- ^ The age of the Sun is around 4.6 billion years.[10]
- ^ The age of the Solar System is 4.532 billion years.
- ^ Neptune is 3.883 times larger than Earth.[23]
- ^ Assuming albedos of 0.6 and 0 respectively.
- ^ Assuming albedos of 0.6 and 0 respectively.
- ^ Assuming an albedo of 0, similar to the measured albedo of TRAPPIST-1b.
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This page was last edited on 21 April 2024, at 23:00