| A remote star with a high luminosity can have the same apparent magnitude as a nearby star with a low luminosity. |
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| Vega has a higher apparent magnitude, while Deneb has a higher absolute magnitude. |
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| The apparent magnitude, m, of a star is a measure of how bright a star appears as observed on or near Earth. |
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| Think about a method to estimate the apparent magnitude, m, using the curves. |
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| This equation establishes the connection between the apparent magnitude, m, the absolute magnitude, M, and the distance, D, measured in parsec. |
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| Knowing the apparent magnitude and the distance of a star, we are able to determine its luminosity. |
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| Having such a metric obviates a major analytic problem caused by discrete characters, which is that units of the same apparent magnitude are not necessarily equivalent. |
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| Astronomers measure the brightness of objects in the sky by their apparent magnitude. |
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| The absolute magnitude, M, is defined as the apparent magnitude a star would have if it were placed 10 parsecs from the Sun. |
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| Instead of defining the apparent magnitude from the number of light photons we observe, it is defined relative to the magnitude and intensity of a reference star. |
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| What George Berkeley calls visible magnitude was by astronomers called apparent magnitude. |
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| Another logarithmic scale is apparent magnitude. |
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| Its apparent magnitude is 1.25 and the distance is 993 parsec. |
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| While looking up at the night sky, the only perceivable difference between stars is their apparent magnitude, but stars each have their own characteristics. |
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| In the visible light, the pulsar is of 16th apparent magnitude. |
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| The absolute magnitude is defined as the apparent magnitude measured at 10 parsecs from the source. |
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