Английская Википедия:HD 147018
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HD 147018 is a star in the southern constellation of Triangulum Australe.[1] It has a yellow-orange hue with an apparent visual magnitude of 8.30,[2] which is too faint to be seen with the naked eye but can be viewed with a small telescope. The star is located at a distance of 132 light years from the Sun based on parallax,[3] but is drifting closer with a radial velocity of −27.5 km/s.[2]
The stellar classification of HD 147018 is G8/K0V[4] or G9V,[5] matching a late G-type main-sequence star that is generating energy through core hydrogen fusion. It is roughly six billion years old and is spinning with a projected rotational velocity of 1.56 km/s. The star has 93%[5] of the mass of the Sun and 94%[3] of the Sun's radius. The metallicity, or abundance of heavier elements, is higher than in the Sun.[5] The star is radiating 71%[3] of the luminosity of the Sun from its photosphere at an effective temperature of 5,441 K.[5]
In August 2009, two extrasolar planets, HD 147018 b and HD 147018 c, were reported to be orbiting this star. The planets were found using the radial velocity method, using the CORALIE spectrograph at La Silla Observatory, Chile.[5]
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See also
References
Шаблон:Sky Шаблон:Stars of Triangulum Australe
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<ref>; для сносокSegransan_et_al_2009не указан текст
- Английская Википедия
- G-type main-sequence stars
- Planetary systems with two confirmed planets
- Triangulum Australe
- Durchmusterung objects
- Henry Draper Catalogue objects
- Hipparcos objects
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- Страницы с телепортом
- Википедия
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