Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Puppis |
Right ascension | 07h 53m 03.63538s[1] |
Declination | −49° 36′ 46.9530″[1] |
Apparent magnitude (V) | 4.63[2] |
Characteristics | |
Spectral type | B2V[3] |
U−B color index | −0.92[2] |
B−V color index | −0.23[2] |
Variable type | Constant[4] |
Astrometry | |
Radial velocity (Rv) | +8.00±4.2[5] km/s |
Proper motion (μ) | RA: −7.77[1] mas/yr Dec.: +15.16[1] mas/yr |
Parallax (π) | 4.30 ± 0.15 mas[1] |
Distance | 760 ± 30 ly (233 ± 8 pc) |
Absolute magnitude (MV) | −2.2±0.1[6] |
Details | |
Mass | 9.6 M☉[7] 10.1±0.5[8] M☉ |
Radius | 4.5±0.7[8] R☉ |
Luminosity | 5,908[9] L☉ |
Surface gravity (log g) | 4.01±0.09[6] cgs |
Temperature | 23,700[9] K |
Metallicity [Fe/H] | +0.01[10] dex |
Rotation | 1.33026 d[11] |
Rotational velocity (v sin i) | 160[12] km/s |
Age | 12.6+7.4 −2.7[8] Myr |
Other designations | |
Database references | |
SIMBAD | data |
HD 64740 is a single[13] star in the southern constellation Puppis, positioned near the line of sight to the Gum Nebula.[4] It has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.63.[2] Parallax measurements give a distance estimate of approximately 760 light-years from the Sun,[1] and it is drifting further away with a radial velocity of +8 km/s.[5]
This is a massive B-type main-sequence star with a stellar classification of B2V.[3] It is a magnetic chemically peculiar star of the helium strong variety[6] with weak hydrogen alpha emission.[8] The polar magnetic field strength is 3,700 G.[4] The star is about halfway through its main sequence lifetime with an estimated age of ~13 million years.[8] It is spinning rapidly with an equatorial velocity of about 140±10 km/s, based on a polar inclination angle of 36°±15°,[4] giving it a rotation period of ~1.33 days.[11] The star is radiating over 5,900 times the luminosity of the Sun from its photosphere at an effective temperature of 23,700 K.[9]
Significant X-ray emission has been detected originating from this star, which may be connected to the magnetically-confined stellar wind.[14] The star does not display pulsation behavior, but it does show a magnetically-modulated variation from the wind.[15] Variation of ultraviolet lines of silicon has been detected, which may be due to surface abundance variations.[4] Two patches of helium overabundance are observed near the magnetic poles, which are inclined by about 20° to the star's pole of rotation.[11]
vanLeeuwen2007
was invoked but never defined (see the help page).Ducati2002
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was invoked but never defined (see the help page).Krtička_et_al_2013
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was invoked but never defined (see the help page).Schulz_et_al_2019a
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was invoked but never defined (see the help page).Hohle2010
was invoked but never defined (see the help page).Gontcharov2012
was invoked but never defined (see the help page).Alecian_et_al_2012
was invoked but never defined (see the help page).Hoffleit1991
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