| 31. | Kosmos 60 measured the gamma-ray background flux density to be 1.7?0 4 quanta / ( m 2 �s ).
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| 32. | AB magnitude is defined so that the zero point corresponds to a bandpass-averaged spectral flux density of 3631 Jansky:
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| 33. | At a point within a collimated beam, the spectral flux density vector has a value equal to the Poynting vector,
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| 34. | Gaussian units, flux density " is " the very same as electric field in free space, not just a scaled copy.
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| 35. | There are two main approaches to definition of the spectral flux density at a measuring point in an electromagnetic radiative field.
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| 36. | This is because the internal magnetic domains of the material align with each other to greatly enhance the magnetic flux density.
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| 37. | This means, that when the product \ sigma \ lambda _ s is positive, the flux density B increases under stress.
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| 38. | Sometimes it is more convenient to display graphical spectra with vertical axes that show the "'relative spectral flux density " '.
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| 39. | In this case, the spectral flux density at a given wavelength is expressed as a fraction of some arbitrarily chosen reference value.
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| 40. | On the other hand, when the product \ sigma \ lambda _ s is negative, the flux density B decreases under stress.
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