Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Coma Berenices |
Right ascension | 12h 39m 21.50369s [1] |
Declination | +20° 01′ 40.0360″ [1] |
Apparent magnitude (V) | 8.43 [2] |
Characteristics | |
Evolutionary stage | Main sequence |
Spectral type | K0V [2] |
Astrometry | |
Radial velocity (Rv) | −8.56±0.13 [1] km/s |
Proper motion (μ) | RA: -81.703 mas/yr [1] Dec.: -104.532 mas/yr [1] |
Parallax (π) | 31.0369 ± 0.0222 mas [1] |
Distance | 105.09 ± 0.08 ly (32.22 ± 0.02 pc) |
Details [3] | |
Mass | 0.798±0.042 M☉ |
Radius | 0.788±0.008 R☉ |
Surface gravity (log g) | 4.54±0.03 cgs |
Temperature | 5266±64 K |
Metallicity [Fe/H] | −0.20±0.04 dex |
Rotational velocity (v sin i) | 2.5±1.0 km/s |
Age | 8.1±4.0 Gyr |
Other designations | |
Database references | |
SIMBAD | data |
Exoplanet Archive | data |
HD 110067 is a star with six known sub-Neptune exoplanets (b, c, d, e, f, g) with radii ranging from 1.94 R⊕ to 2.85 R⊕. The planets orbit the host star in a rhythmic orbital resonance. The star, and related planetary system, is located 105 light-years away in the constellation Coma Berenices. [3] [4] [5] [6] [7] [8] [9] [10]
HD 110067 is part of a wide triple star system, along with the spectroscopic binary system HD 110106. [11]
HD 110067, located 105 light-years away in the constellation Coma Berenices, is orbited by six known sub-Neptune exoplanets (b, c, d, e, f, g) with radii ranging from 1.94 R⊕ to 2.85 R⊕, and with densities (and solid cores) similar to that of gas giants in the Solar System. None of the planets in the planetary system were found to be in the habitable zone for life as we know it. [8]
The two innermost exoplanets orbiting HD 110067, a bright K0-type star, were first detected by the TESS (NASA) space telescope, using the transit method, in 2020. The remaining four exoplanets were later confirmed in 2023 as a result of additional observations using the CHEOPS (European Space Agency) space telescope. [9]
On 29 November 2023, an international team of astronomers, led by Rafael Luque, astronomer from the University of Chicago, published a review of the discovery in the journal Nature entitled, "A resonant sextuplet of sub-Neptunes transiting the bright star HD 110067". [3] According to Luque, "It’s like looking at a fossil: The orbits of the planets today are the same as they were a billion years ago." [9]
Further study of the HD 110067 planetary system may provide a better understanding of how the pattern of the planetary orbits in the Solar System arose, which once may have begun harmoniously, but later turned chaotic. The result, possibly, of a passing star or planet or some other astronomical object capable of disrupting the nascent harmonic orbital dynamics. Additionally, further studies of the system, including compositional studies of the planetary interiors and atmospheres, may also provide a better understanding of the conditions that potentially may support life. [9]
Six known sub-Neptune exoplanets (b, c, d, e, f, g) with planetary radii ranging from 1.94 R⊕ to 2.85 R⊕ from HD 110067, the host star. All planets are smaller than Neptune and have large atmospheres. The star and related planetary system are located 105 light years away, in the constellation Coma Berenices. Masses of all six of the planets in the system range from 3.9 M⊕ (mass of Earth) to 8.5 M⊕. All of the planetary orbits in the HD 110067 system are closer to their star than distance between the planet Mercury and the Sun. [3] [4]
The planets orbit the host star in synchronized rhythms of orbital resonance (a rare 1 percent of such systems in the Milky Way galaxy have this symmetry): the innermost planet orbits three times for every two times for the next planet out – a so-called 3:2 resonance; this same 3:2 resonance also applies to the second and third planet, as well as to the third and fourth planet; whereas the fourth planet orbits four times for every three times for the fifth planet out – in a so-called 4:3 resonance; additionally, the penultimate fifth planet orbits the sixth planet out in this same 4:3 resonance. Further, the innermost planet completes six orbits in exactly the same time the outermost planet completes one orbit. [3] [4] [5] [6] [7] [8] [9] [10]
The resonance ratio for the entire system is 54:36:24:16:12:9. [3] [4] The resonance period is ~492 d⊕ (Earth-days).[ citation needed ]
Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | 5.69+1.78 −1.82 M🜨 | 0.0793±0.00096 | 9.113678(10) | — | 89.061±0.099 ° | 2.200±0.030 R🜨 |
c | < 6.3 M🜨 | 0.1039±0.0013 | 13.673694(24) | — | 89.687±0.163 ° | 2.388±0.036 R🜨 |
d | 8.52+3.31 −3.25 M🜨 | 0.1362±0.0017 | 20.519617(40) | — | 89.248±0.046 ° | 2.852±0.039 R🜨 |
e | < 3.9 M🜨 | 0.1785±0.0022 | 30.793091(12) | — | 89.867±0.089 ° | 1.940±0.040 R🜨 |
f | 5.04+1.89 −1.94 M🜨 | 0.2163±0.0026 | 41.05854(10) | — | 89.673±0.046 ° | 2.601±0.042 R🜨 |
g | < 8.4 M🜨 | 0.2621±0.0032 | 54.76992(20) | — | 89.729±0.073 ° | 2.607±0.052 R🜨 |
In celestial mechanics, orbital resonance occurs when orbiting bodies exert regular, periodic gravitational influence on each other, usually because their orbital periods are related by a ratio of small integers. Most commonly, this relationship is found between a pair of objects. The physical principle behind orbital resonance is similar in concept to pushing a child on a swing, whereby the orbit and the swing both have a natural frequency, and the body doing the "pushing" will act in periodic repetition to have a cumulative effect on the motion. Orbital resonances greatly enhance the mutual gravitational influence of the bodies. In most cases, this results in an unstable interaction, in which the bodies exchange momentum and shift orbits until the resonance no longer exists. Under some circumstances, a resonant system can be self-correcting and thus stable. Examples are the 1:2:4 resonance of Jupiter's moons Ganymede, Europa and Io, and the 2:3 resonance between Neptune and Pluto. Unstable resonances with Saturn's inner moons give rise to gaps in the rings of Saturn. The special case of 1:1 resonance between bodies with similar orbital radii causes large planetary system bodies to eject most other bodies sharing their orbits; this is part of the much more extensive process of clearing the neighbourhood, an effect that is used in the current definition of a planet.
55 Cancri is a binary star system located 41 light-years away from the Sun in the zodiac constellation of Cancer. It has the Bayer designation Rho1 Cancri (ρ1 Cancri); 55 Cancri is the Flamsteed designation. The system consists of a K-type star and a smaller red dwarf.
Hot Jupiters are a class of gas giant exoplanets that are inferred to be physically similar to Jupiter but that have very short orbital periods. The close proximity to their stars and high surface-atmosphere temperatures resulted in their informal name "hot Jupiters".
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This page describes exoplanet orbital and physical parameters.
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An exoplanet is a planet located outside the Solar System. The first evidence of an exoplanet was noted as early as 1917, but was not recognized as such until 2016; no planet discovery has yet come from that evidence. What turned out to be the first detection of an exoplanet was published among a list of possible candidates in 1988, though not confirmed until 2003. The first confirmed detection came in 1992, with the discovery of terrestrial-mass planets orbiting the pulsar PSR B1257+12. The first confirmation of an exoplanet orbiting a main-sequence star was made in 1995, when a giant planet was found in a four-day orbit around the nearby star 51 Pegasi. Some exoplanets have been imaged directly by telescopes, but the vast majority have been detected through indirect methods, such as the transit method and the radial-velocity method. As of 24 July 2024, there are 7,026 confirmed exoplanets in 4,949 planetary systems, with 1007 systems having more than one planet. This is a list of the most notable discoveries.
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