HD 97048
Herbig Ae/Be star in the constellation Chamaleon
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HD 97048 or CU Chamaeleontis is a Herbig Ae/Be star 603 ly away in the constellation Chamaeleon. It is a variable star embedded in a dust cloud containing a stellar nursery, and is itself surrounded by a dust disk.
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Chamaeleon[1] |
| Right ascension | 11h 08m 03.31097s[2] |
| Declination | −77° 39′ 17.4908″[2] |
| Apparent magnitude (V) | 8.38 - 8.48[3] |
| Characteristics | |
| Evolutionary stage | Herbig Ae/Be[4] |
| Spectral type | A0Vep[5] |
| Variable type | INA[3] |
| Astrometry | |
| Radial velocity (Rv) | +34.00±2.5[6] km/s |
| Proper motion (μ) | RA: −22.526 mas/yr[2] Dec.: +1.291 mas/yr[2] |
| Parallax (π) | 5.4228±0.0249 mas[2] |
| Distance | 601 ± 3 ly (184.4 ± 0.8 pc) |
| Absolute magnitude (MV) | +2.47[1] |
| Details | |
| Mass | 2.5[4] M☉ |
| Radius | 1.7[7] R☉ |
| Luminosity | 33[7] L☉ |
| Surface gravity (log g) | 4.30[7] cgs |
| Temperature | 10,500[7] K |
| Age | 3[4] Myr |
| Other designations | |
| CD−76 488, HIP 54413, SAO 256802[8] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HD 97048 is a young star still contracting towards the main sequence. Its brightness varies between magnitudes 8.38 and 8.48 and it is classified as an Orion variable.[3] It was given the variable star designation CU Chamaeleontis in 1981.[9] Its spectrum is also variable. The spectral class is usually given as A0 or B9, sometimes with a giant luminosity class, sometimes main sequence. The spectrum shows strong variable emission lines indicative of a shell surrounding the star.[5]
HD 97048 is a member of the Chamaeleon T1 stellar association and is still embedded within the dark molecular cloud that it is forming from. It illuminates a small reflection nebula against the dark cloud.[10]
Planetary system
This star has a substantial dust disk having a central cavity with a 40−46 AU radius[4] The disk has a carbon monoxide gas velocity kink and intensity gap at 130 AUs, which is suspected to be caused by a superjovian planet.[11] In 2019, HCO+ ion and Hydrogen cyanide emission was detected from the disk, suggesting a large amount of gas is orbiting beyond 200 AU radius.[12]
In the system a kink in the velocity of carbon monoxide gas (CO 3–2) as well as a gap in the dust emission of the disk are seen as evidence for a jovian protoplanet. The protoplanet is located at 130 au from the star and has a mass of about 2.5 Jupiter masses. It is one of the lowest mass protoplanets discovered as of 2023.[11]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| protoplanetary disk | 40–850 AU | 40° | — | |||
| b | 2.5±0.5 MJ | 130 | — | — | 40° | — |