A comparison between the night sky of Earth and a planet of HD 69830.
08h18m23.9s, −12° 37′ 55.0″| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Puppis |
| Right ascension | 08h18m 23.94697s[1] |
| Declination | −12° 37′ 55.8172″[1] |
| Apparent magnitude (V) | +5.98[2] |
| Characteristics | |
| Spectral type | G8V[3] |
| U−B color index | 0.33[2] |
| B−V color index | 0.75[2] |
| V−R color index | 0.40 |
| R−I color index | 0.36 |
| Variable type | none |
| Astrometry | |
| Radial velocity (Rv) | 30.09±0.12[1] km/s |
| Proper motion (μ) | RA: 278.790 mas/yr[1] Dec.: −987.829 mas/yr[1] |
| Parallax (π) | 79.4953 ± 0.0400 mas[1] |
| Distance | 41.03 ± 0.02 ly (12.579 ± 0.006 pc) |
| Absolute magnitude (MV) | 5.47 ± 0.01[4] |
| Details | |
| Mass | 0.89 ± 0.03[5] M☉ |
| Radius | 0.905 ± 0.019[3] R☉ |
| Luminosity | 0.622 ± 0.014[3] L☉ |
| Surface gravity (log g) | 4.53[6] cgs |
| Temperature | 5,394 ± 62[3] K |
| Metallicity [Fe/H] | −0.04 ± 0.03[3] dex |
| Rotation | 35.1 ± 0.8 days[7] |
| Rotational velocity (v sin i) | 0.8±0.5[3] km/s |
| Age | 10.6 ± 4[3] Gyr |
| Other designations | |
285 G. Puppis,[8] BD−12°2449, GJ 302, HIP 40693, HR 3259, LHS 245, SAO 154093, 2MASS J08182389-1237541, Gaia DR2 5726982995343100928[9] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| ARICNS | data |
HD 69830 (285 G. Puppis) is a yellow dwarf star located 41.0 light-years (12.6 parsecs) away in the constellationofPuppis. In 2005, the Spitzer Space Telescope discovered a narrow ring of warm debris orbiting the star.[10] The debris ring contains substantially more dust than the Solar System's asteroid belt. In 2006, three extrasolar planets with minimum masses comparable to Neptune were confirmed in orbit around the star, located interior to the debris ring.[11]
HD 69830 is a main sequence star of spectral type G8V. It has about 86% of the Sun's mass, 90% of its radius, 62% of its luminosity, and 89% of its iron abundance. The star's age has been estimated at 10.6 ± 4 billion years. HD 69830 is located about 40.7 light-years from the Sun, lying in the northeastern part of the constellationofPuppis (the Poop Deck). It can be seen east of Sirius, southwest of Procyon, northeast of Delta Canis Majoris, and north of Zeta Puppis.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥10.1+0.38 −0.37 M🜨 |
0.0764±0.0017 | 8.66897±0.00028 | 0.128±0.028 | — | — |
| c | ≥12.09+0.55 −0.54 M🜨 |
0.181±0.004 | 31.6158±0.0051 | 0.03±0.027 | — | — |
| d | ≥12.26+0.89 −0.88 M🜨 |
0.622±0.014 | 201.4±0.4 | 0.08±0.071 | — | — |
| Asteroid belt | 0.93–1.16 AU | — | — | |||
On May 17, 2006, a team of astronomers using the European Southern Observatory's (ESO) HARPS spectrograph on the 3.6-metre La Silla telescope in the Atacama desert, Chile, announced the discovery of three extrasolar planets orbiting the star. With minimum masses between 10 and 18 times that of the Earth, all three planets are presumed to be similar to the planets NeptuneorUranus.[11] As of 2011[update], no planet with more than half the mass of Jupiter had been detected within three astronomical units of HD 69830.
The star rotates at an inclination of 13+27
−13 degrees relative to Earth.[7] It has been assumed that the planets share that inclination.[13] However b and c are "hot Neptunes", and outside this system several are now known to be oblique relative to the stellar axis.[14]
The outermost planet discovered appears to be within the system's habitable zone, where liquid water would remain stable (more accurate data on the primary star's luminosity will be required to know for sure where the habitable zone is). HD 69830 is the first extrasolar planetary system around a Sun-like star without any known planets comparable to JupiterorSaturninmass.[11]
The planetary parameters were updated in 2023.[5]
In 2005, the Spitzer Space Telescope detected a debris disk in the HD 69830 system consistent with being produced by an asteroid belt twenty times more massive than that in our own system. The belt was originally thought to be located inside an orbit equivalent to that of Venus in the Solar System, which would place it between the orbits of the second and third planets. The disk contains sufficient quantities of dust that the nights on any nearby planets would be lit up by zodiacal light 1000 times brighter than that seen on Earth, easily outshining the Milky Way.
Further analysis of the spectrum of the dust revealed that it is composed of highly processed material, likely derived from a disrupted C-type asteroid of at least 30 km radius which contained many small olivine-rich (rocky) and once-wet grains which would not survive at close distances to the star. Instead, it seems more likely that the asteroid belt producing the dust is located outside the orbit of the outermost planet, around 1 AU from the star. This region contains the 2:1 and 5:2 mean motion resonances with HD 69830 d.[12]
{{cite web}}: CS1 maint: postscript (link)
