Übersetzung für "Scheinbaren helligkeit" in Englisch

It has a visual magnitude of 8.8v and photographic magnitude of 9.7p.

Because of its apparent magnitude, the star cannot be seen with the naked eye.

The apparent magnitude of this star is 12.51, so it cannot be seen with the unaided eye.

It is classified as a semiregular variable star and its brightness varies from magnitude 2.99m to 3.33m.

It is one of the few O-class stars that are visible to the unaided eye.

At apparent magnitude 15.1, it is too faint to be seen with the unaided eye.

This in turn provides a distance estimate to the cluster, based on the visual magnitude of the stars.

This is a suspected variable star with an apparent magnitude that may rise as high as 2.76.

The apparent magnitude of this star is 12.51, so it cannot be seen with the unaided eye.

With an apparent magnitude of -1.6 it is the brightest star of the entire night sky.

With an apparent visual magnitude of 2.0, it is among the brightest stars in the night sky.

With an apparent visual magnitude of 7.34, this star is too faint to be viewed with the naked eye even under excellent seeing conditions.

By comparing this known luminosity to an object's observed brightness, the distance to the object can be computed using the inverse square law.

However with an apparent magnitude of about 8.5 it is too faint to be seen without a telescope.

With an apparent visual magnitude of 14.81, it is much too faint to be seen with the naked eye.

Even though it is a relatively nearby it is very dim with a magnitude of about 13 so it can only be seen with at least a moderately-sized telescope.

As all the stars of a globular cluster are at approximately the same distance from the Earth, their absolute magnitudes differ from their visual magnitude by about the same amount.

During the closest approach the comet appeared as a circular cloud about the size of the full moon, having no discernible tail, and shining at a naked eye magnitude of 3-4.

Nu¹ Sagittarii A is a spectral type K1 bright giant which has an apparent magnitude of +4.86.

Lambda Boötis is a white A-type main sequence dwarf with an apparent magnitude of +4.18.

Essentially, the Hertzsprung-Russell diagram gives us the information we missed: the absolute brightnesses of the stars for which we can only observe their apparent brightnesses.

Evolution of the apparent brightness of the central star as planet WTS-1b passes in front of it causing an eclipse

While at the Observatory he worked on ways to determine the apparent brightness of stars using photographic plates:

From its apparent size and magnitude, M62 is very similar to its neighbor, M19. Physically, they are a bit less similar because their distances are somewhat different different: M62 is at 22,500, M19 at 28,400 light years, according to W.E. Harris' database.

The planetoid Vesta, which was discovered as fourth planetoid, is located at the north-west corner of the open star cluster Collinder 65 in the constellation taurus and with an apparent brightness of 8.5mag you can observe it - like Ceres - with binoculars. It is located in the same region like Ceres, near crab nebula(M1). It can be found after midnight over the eastern horizon and can be observed till morning dawn: