Question

What is the method of measuring distance to stars beyond 100 years?
A. Cepheid variable stars
B. Heid variable stars
C. Lowheid variable stars
D. None

Answer 1

Hint: A variable star is a star whose brightness as seen from Earth (its apparent magnitude) fluctuates.
A rotating star is a star that shines with its fluctuating brightness as seen on Earth (its apparent size).

Complete step by step solution:
These variations can be caused by a change in emitted light or by something else blocking the light, the variable stars are classified as:
Intrinsic variability, its changing brightness in fact; for example, because a star swells from time to time and shrinks.
Extreme variability, the changes in light are due to changes in the amount of light that can reach Earth; for example, because a star has a more orbiting counterpart sometimes.
Cepheid variables have several types of striking stars, all of which are found in the line of instability and constant decrease due to the star's own weight, usually a basic frequency. The Eddington valve process of pulsating variables is generally believed to cause cepheid-like strokes. Each group in the line of instability has a fixed relationship between time and absolute magnitude, as well as the relationship between the period and the number of stars.
Over 100 light years, the distance is measured using a change in starlight.
Complete step by step solution:
The method of measuring the distance of stars beyond 100 light years is to use Cepheid variable stars. These stars change in brightness over time, which allows astronomers to figure out the true brightness.

Note: Cepheid variable is a sort of star that throbs radially, shifting in both breadth and temperature and creating changes in splendor with an all around characterized stable period and wavelength. A solid direct connection between a Cepheid variable's glow and throb period set up Cepheid as significant markers of infinite benchmarks for scaling galactic and extragalactic distances. This powerful quality of old style Cepheid was found in 1908 by Henrietta Swan Leavitt subsequent to considering a great many variable stars in the Magellanic Clouds. This disclosure permits one to know the genuine radiance of a Cepheid by basically noticing its throb period. This thus permits one to decide the distance to the star, by contrasting its known radiance with its noticed brilliance.