Introduction
Two stars on the Hero map: The blue area of the standard RR represents the Tianqin Ratch RR-shaped star, the red area of the standard C represents the parent variety. Tian Qin RR-type starry star, also known as the star group, is one of the pulsating star, has a weighing relationship (but not obvious) similar to the parent variety of stars, which can be used to determine the distance. The brightest in this type of thorough is the Neiqin RR star, and therefore name.
Most pulsating stars are located on a narrow instability belt on the Herrot, which is located in the middle and lower part of this unstable band, which is mostly a type A, small portion is F type. Almost the same absolute star, etc. Because Tianqin RR-type starry is found in the horizontal branch of the spherical star, it is also known as the star group. The total number of Tianqin Rat RR-shaped shadows that have been discovered is about 1/4 of pulsating star.
The position of the two stars on the Herrot map: the blue area of the standard RR represents the Niangjian RR-shaped star, the red area of the standard C represents the parent variety. Tian Qin RR-type starry star, also known as the star group, is one of the pulsating star, has a weighing relationship (but not obvious) similar to the parent variety of stars, which can be used to determine the distance. The brightest in this type of thorough is the Neiqin RR star, and therefore name. The RRAB type light change curve is asymmetrical, and the optical change cycle is relatively long (an average of 0.5 days), which is relatively large (greater than 0.5, etc.), and the RRC type light curve is almost symmetrical, close to the sinusoidal curve, and the optical change cycle A shorter (an average of 0.3 days), the expiration is relatively small (less than 0.5, etc.).
Distribution
The Tianqin Rat in the Milky Way is widely distributed in the silver surface, the silver and spherical clusters. Because they are relatively high, it is easier to identify and observe. Tianqin Rat RR-type threshold can be used to determine the gaussic spherical star group and the distance adjacent to the galaxy, which lays the foundation for the study of the age, star evolution of the spheroid group, and the dynamics and evolution of Military and evolution. Independent checks can also be independently validated.
This variation range of this starry star and its smaller quality (usually only 60% -80% of the sun) prove that they are older stars. Some even reached 12 billion, almost and the same age. They have a large radius, usually 4-6 times the sun, so the photome is still bright. These stars are templates for the late stage of medium and medium quality star evolution. They have passed the red superstar stage, gradually contracted heat, will eventually become a hot white dwarf.