Ross 154 – a star in the southern zodiac constellation of Sagittarius

Ross 154 (also named V1216 Sgr) is a star in the southern zodiac constellation of Sagittarius. This dim star is the seventh closest to our Sun, lying at about 9.7 light-years (ly) away. It has an apparent magnitude of 10.44, so it is much too faint to be seen with the naked eye. The distance to this star can be estimated from parallax measurements, which places it at 9.69 light-years (2.97 parsecs) away from Earth. It is the nearest star in the southern constellation Sagittarius, and one of the closest to the Sun. However, Ross 154 is too faint to be seen by the naked eye.

Ross 154 is a star in the Alpha Quadrant that was located approximately ten light years from Sol.

This star was first cataloged by American astronomer Frank Elmore Ross in 1925. Ross 154 was found to be a UV Ceti-type flare star, with a mean time between major flares of about two days. The first such flare activity was observed from Australia in 1951 when the star increased in magnitude by 0.4. Usually, the star will increase by 3–4 magnitudes during a flare. The quiescent X-ray luminosity is about 9 × 1027 ergs s-1. X-ray flare emission from this star has been observed by Chandra observatory, with a particularly large flare emitting 2.3 × 1033 erg.

Ross 154 is an X-ray source and it has been detected by several X-ray observatories. The first such flare activity was observed from Australia in 1951 when the star increased in magnitude by 0.4. The quiescent X-ray luminosity is about 9 × 1027 ergs s−1. Typically, the star will increase by 3-4 magnitudes during a flare. The strength of the star’s surface magnetic field is an estimated 2.2 ± 0.1 kG. X-ray flare emission from this star has been observed by Chandra observatory, with a particularly large flare emitting 2.3 × 1033 erg. Ross 154 is an X-ray source and it has been detected by several X-ray observatories.

Ross 154 was found to be a UV Ceti-type flare star, with a mean time between major flares of about two days. This is a red dwarf star that is generating energy through the nuclear fusion of hydrogen at its core. It has an estimated 17% of the Sun’s mass and 24% of the Sun’s radius, but it is radiating only 0.38% of the luminosity of the Sun.

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