cepheid variable

It belongs to an unusual class of stars called Cepheid variables.

He began this in 1916 with investigations of possible physical explanations for Cepheid variables.

Leavitt focused on a type of star known as a Cepheid variable.

These stars are somewhat similar to Cepheid variables, but they do not have the same relationship between their period and luminosity.

This discovery became known as the "period-luminosity relationship" of Cepheid variables.

"It is, after all, one of the larger Cepheid variables in Federation space."

Astronomers used nearly 50 Cepheid variables in this galaxy to determine its distance to be 108 million light years.

This measurement is completely independent of traditional measurements using Cepheid variables and other techniques.

Cepheid variables reside in the upper section of the instability strip.

That this is not merely a philosophical issue can be seen from the history of distance measurements using Cepheid variables.

Oscillations at this frequency are seen in Cepheid variables.

So another type of "standard candle" - one vastly brighter than the Cepheid variables - is needed.

The project also checked to see if the properties of Cepheid variables are sensitive to stellar composition.

"Yes, but these instruments don't know any better since they're judging by strictly physical guideposts like Cepheid variables."

Cepheid variables are a class of stars with a luminosity that changes as a function of time.

Being a lenticular galaxy, it is not suitable to apply the cepheid variable method.

Its outer arms have a high number of Cepheid variables, which are used as standard candles to determine astronomical distances.

Historically time domain astronomy has come to include appearance of comets, and cepheid variable.

Ashbrook was one of the first to study Cepheid variables as tools for establishing galactic distances.

Cepheid variables are used to establish the distance to the Galactic center, globular clusters, and galaxies.

It is a classic Cepheid variable, the closest to us in the whole Milky Way.

They exhibit relationships between their periods, masses, and luminosity, although not with the precision of more conventional Cepheid variables.

First he measured thirteen nearby cepheid variables to find the absolute magnitude of a variable with a period of one day.

It is a cepheid variable.

Delta Cephei is a classical, or type I, Cepheid variable.