intrinsic luminosity

To determine the intrinsic luminosity of a star requires knowledge of its distance.

The higher sorts of deva shine with their own intrinsic luminosity.

Sirius appears bright because of both its intrinsic luminosity and its proximity to Earth.

The relation enables the difficult-to-observe intrinsic luminosity to be calculated from the relatively easily-observable velocity.

Using such techniques, astronomers can estimate the intrinsic luminosity of a gamma ray burst within 25 percent, Dr. Lamb said.

Another method is to measure the brightness of an object and assume an intrinsic luminosity, from which the distance may be determined using the inverse square law.

This measurement was based primarily on observations of Cepheid stars, objects of known intrinsic luminosity that have acted as cosmic mileposts this century.

The Universe Could Collapse Astronomers rely on certain "standard candles," or objects whose intrinsic luminosity is reasonably well known, in trying to measure cosmic distances.

The lensing hypothesis greatly reduces the intrinsic luminosity of the lensed quasar as the observed brightness is enhanced by the magnification effect of the lens.

After further study, she confirmed in 1912 that the Cepheid variables with greater intrinsic luminosity did have longer periods, and that the relationship was quite close and predictable.

When astronomers wish to trace the evolution of stars, they will most likely turn to a graph that plots the intrinsic luminosity of a star against its surface temperature or spectral type.

If the intrinsic luminosity of a distant object is known, we can calculate its luminosity distance by measuring the flux and determine , which turns out to be equivalent to the expression above.

Since all Type Ia supernovae are believed to occur in essentially the same way, they form a standard candle whose intrinsic luminosity can be assumed to be approximately the same in all cases.

The distance from Kepler-16 to Earth has not been measured, but is probably about 200 light years, judging from the apparent brightness of star A and theoretical models of stellar structure that give a crude estimate of its intrinsic luminosity.

Her discovery is known as the "period-luminosity relationship": The logarithm of the period is linearly related to the star's average, intrinsic luminosity (which is defined as a logarithm of the amount of power radiated by the star in the visible spectrum).

In astronomy, the Tully-Fisher relation, published by astronomers R. Brent Tully and J. Richard Fisher in 1977, is an empirical relationship between the intrinsic luminosity (proportional to the stellar mass) of a spiral galaxy and its velocity width (the amplitude of its rotation curve).