 A light curve for 44 Boötis plotted from TESS data | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Boötes |
| Right ascension | 15 03 47.29565 |
| Declination | +47° 39′ 14.6228″ |
| Apparent magnitude (V) | 4.70 - 4.84 (5.136 / 6.004) |
| Characteristics | |
| Spectral type | G0Vnv + (K0V + K4V) |
| U−B color index | 0.09 |
| B−V color index | 0.65 |
| Variable type | W UMa |
| Astrometry | |
| Radial velocity (Rv) | −17.89 km/s |
| Proper motion (μ) | RA: −445.84 mas/yr Dec.: 19.86 mas/yr |
| Parallax (π) | 78.39 ± 1.03 mas |
| Distance | 41.6 ± 0.5 ly (12.8 ± 0.2 pc) |
| Absolute magnitude (MV) | +2.211 / +5.38 |
| Orbit | |
| Primary | 44 Boo A |
| Companion | 44 Boo B |
| Period (P) | 209.8±3.3 yr |
| Semi-major axis (a) | 3.666±0.021″ |
| Eccentricity (e) | 0.5111±0.0065 |
| Inclination (i) | 83.55±0.05° |
| Longitude of the node (Ω) | 57.14±0.06° |
| Periastron epoch (T) | B 2012.04±0.26 |
| Argument of periastron (ω) (secondary) | 39.86±0.68° |
| Orbit | |
| Primary | 44 Boo Ba |
| Companion | 44 Boo Bb |
| Period (P) | 0.267818 days |
| Semi-major axis (a) | 2.015 R☉ |
| Eccentricity (e) | 0.0 |
| Inclination (i) | 72.8° |
| Semi-amplitude (K1) (primary) | 231.31 km/s |
| Semi-amplitude (K2) (secondary) | 112.70 km/s |
| Details | |
| 44 Boo A | |
| Mass | 1.04±0.10 M☉ |
| Luminosity | 1.552 L☉ |
| Surface gravity (log g) | 4.33 cgs |
| Temperature | 5,877 K |
| Metallicity | −0.24 dex |
| Age | 1.4–1.5 Gyr |
| 44 Boo BA | |
| Mass | 0.98 M☉ |
| Radius | 0.87 R☉ |
| Luminosity | 0.51 L☉ |
| Temperature | 5,300 K |
| 44 Boo Bb | |
| Mass | 0.55 M☉ |
| Radius | 0.66 R☉ |
| Luminosity | 0.24 L☉ |
| Temperature | 5,035 K |
| Other designations | |
| i Boötis, 40 Boo, BD+48°2259, FK5 3182, GJ 575, HD 133640, HIP 73695, HR 5618, SAO 45357, ADS 9494, CCDM 15038+4739 | |
| Database references | |
| SIMBAD | data |
| A | |
| B | |
44 Boötis or i Boötis is a triple star system in the constellation Boötes. It is approximately 41.6 light years from Earth.
44 Boötis can be resolved into two stars, of 5th and 6th magnitudes respectively. They were separated by 1.5″ when the pair were confirmed in 1819, but were only 0.2″ by 2020 as the two orbit every 210 years.
The primary component, 44 Boötis A, is a yellow-white G-type main sequence dwarf with a mean apparent magnitude of +4.83. The companion component, 44 Boötis B, is a W Ursae Majoris variable spectroscopic binary. The variability of this star system was discovered by English astronomer William Herschel. The brightness of the eclipsing binary varies from magnitude +5.8 to +6.40 with a period of 6.43 hours. The two eclipsing components of the system are close enough to allow their stellar envelopes to overlap, or at least nearly so. In 1948, flare behavior was measured from this system based on data from O. J. Eggen.
The 44 Boötis system is 42 light-years (13 parsecs) from Earth. It also may show signs of an infrared excess, implying the existence of a dust disk that absorbs visible light and re-emits it as infrared light. The dust would have a blackbody temperature of about 23 K, situated up to 182 au from the parent star.
References
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