DI Chamaeleontis
Star in the constellation Chamaleon
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DI Chamaeleontis, also known as Hen 3-593 or HIP 54365, is a quadruple star system in the constellation Chamaeleon. The system is located 616 light years away from Earth based on Gaia DR3 parallax measurements.[1]
 Image showing DI Cha A and B, each of which is also an even closer binary, and the surrounding nebulosity. | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Chamaeleon |
| A | |
| Right ascension | 11h 07m 20.72761s[1] |
| Declination | −77° 38′ 07.3081″[1] |
| Apparent magnitude (V) | 10.72[2] |
| A | |
| Right ascension | 11h 07m 20.18917s[3] |
| Declination | −77° 38′ 11.5657″[3] |
| Apparent magnitude (V) | 16.7[2] |
| Characteristics | |
| Spectral type | G0e[4] (G2 + M6 + M5.5 + M5.5)[5] |
| U−B color index | +0.630[6] |
| B−V color index | +1.144[6] |
| Variable type | T Tau[7] |
| Astrometry | |
| A | |
| Radial velocity (Rv) | +12.040±0.140[8] km/s |
| Proper motion (μ) | RA: −22.552 mas/yr[1] Dec.: +1.214 mas/yr[1] |
| Parallax (π) | 5.2913±0.0133 mas[1] |
| Distance | 616 ± 2 ly (189.0 ± 0.5 pc) |
| B | |
| Radial velocity (Rv) | +15.5±0.3[9] km/s |
| Proper motion (μ) | RA: −21.477 mas/yr[3] Dec.: +1.289 mas/yr[3] |
| Parallax (π) | 5.2190±0.0719 mas[3] |
| Distance | 625 ± 9 ly (192 ± 3 pc) |
| Details[10] | |
| Aa | |
| Mass | 1.7 M☉ |
| Radius | 2.00 R☉ |
| Luminosity | 4.7 L☉ |
| Temperature | 6,030 K |
| Age | 7.1 Myr |
| Ba/Bb | |
| Mass | 0.18 M☉ |
| Radius | 1.13 R☉ |
| Luminosity | 0.11 L☉ |
| Temperature | 3,130 K |
| Age | 3.0 Myr |
| Other designations | |
| DI Cha, HIP 54365, CD−76°486, WDS J11073-7738, AAVSO 1104-77 | |
| Database references | |
| SIMBAD | data |
| B | |
DI Cha is a variable star of the T Tauri type, young stellar objects just approaching the main sequence. It varies erratically between visual magnitudes 10.65 and 10.74.[7] Although it is visually faint, it was noticed because of the prominent emission lines in its spectrum.[12]
In 1977, DI Cha was observed to have a much fainter companion.[13] The separation was later measured at 4.6", approximately 644 astronomical units (AU).[14] The B component was discovered to be a pair of stars separated by only 0.066", about 10 AU,[15] both with spectral type M5.5.[5] Finally, the variable primary star was found to have a faint companion 0.2" (therefore ~30 AU) away, of spectral type M6.[5]