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Match the following techniques for determining the distances to astronomical bodies to the descriptions: v Radar Ranging v Trigonometric Parallax A. Uses shifting perspective to measure how the foreground objects shift relative to objects in the background. The effects are more noticeable the longer the baseline between the two observation points (ie. moving from one side of the Sun to the other) B. The process or relying on a relation between a star's period of pulsation and its overall luminosity to provide its absolute magnitude, which then can be paired with the observed apparent magnitude to work out the distance modulus and physical distance to the star. Spectroscopic Parallax v Main sequence fitting v Variable Stars C. The process of fitting an observed variation in brightness as the light of this standard candle dims over time to models that can provide the event's absolute magnitude. Once we have the absolute and apparent magnitude, we apply the distance modulus formula to find the physical distance. v Supemova v Hubble's Law D. Measuring distance by measuring the length of time that it takes for radiation to reflect off of a target and return to a detector on Earth. That time is then divided by 2 and multiplied by the speed of light to get the one-way distance. E. We measure the recessional velocities of galaxies and divide that speed by the rate at which the space between galaxies expands per megaparsec to determine the number of megaparsecs between own galaxy and the one we observed. F. The process of measuring the absolute magnitudes of a cluster of stars by aligning them with a portion of the H-R diagram and then pairing that information with their apparent magnitudes to work out the distance modulus and physical distance to the stars. G. Done by fitting a star's spectrum to that of similar stars on the H-R diagram. Doing so provides the star's expected absolute magnitude which, when paired with the star's observed apparent magnitude, allows the observer to apply the distance modulus formula to gather the physical distance to the star.

Match the following techniques for determining the distances to astronomical bodies to the descriptions: v Radar Ranging v Trigonometric Parallax A. Uses shifting perspective to measure how the foreground objects shift relative to objects in the background. The effects are more noticeable the longer the baseline between the two observation points (ie. moving from one side of the Sun to the other) B. The process or relying on a relation between a star's period of pulsation and its overall luminosity to provide its absolute magnitude, which then can be paired with the observed apparent magnitude to work out the distance modulus and physical distance to the star. Spectroscopic Parallax v Main sequence fitting v Variable Stars C. The process of fitting an observed variation in brightness as the light of this standard candle dims over time to models that can provide the event's absolute magnitude. Once we have the absolute and apparent magnitude, we apply the distance modulus formula to find the physical distance. v Supemova v Hubble's Law D. Measuring distance by measuring the length of time that it takes for radiation to reflect off of a target and return to a detector on Earth. That time is then divided by 2 and multiplied by the speed of light to get the one-way distance. E. We measure the recessional velocities of galaxies and divide that speed by the rate at which the space between galaxies expands per megaparsec to determine the number of megaparsecs between own galaxy and the one we observed. F. The process of measuring the absolute magnitudes of a cluster of stars by aligning them with a portion of the H-R diagram and then pairing that information with their apparent magnitudes to work out the distance modulus and physical distance to the stars. G. Done by fitting a star's spectrum to that of similar stars on the H-R diagram. Doing so provides the star's expected absolute magnitude which, when paired with the star's observed apparent magnitude, allows the observer to apply the distance modulus formula to gather the physical distance to the star.

Applications and Investigations in Earth Science (9th Edition)
Applications and Investigations in Earth Science (9th Edition)
9th Edition
ISBN:9780134746241
Author:Edward J. Tarbuck, Frederick K. Lutgens, Dennis G. Tasa
Publisher:Edward J. Tarbuck, Frederick K. Lutgens, Dennis G. Tasa
Chapter1: The Study Of Minerals
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QUESTION 19 Match the following techniques for determining the distances to astronomical bodies to the descriptions: v Radar Ranging A. Uses shifting perspective to measure how the foreground objects shift relative to objects in the background. The effects are more noticeable the longer the baseline between the two observation points (i.e. moving from one side of the Sun to the other) v Trigonometric Parallax v Spectroscopic Parallax B. The process or relying on a relation between a star's period of pulsation and its overall luminosity to provide its absolute magnitude, which then can be paired with the observed apparent magnitude to work out the distance modulus and physical distance to the star. v Main sequence fitting v Variable Stars C. The process of fitting an observed variation in brightness as the light of this standard candle dims over time to models that can provide the event's absolute magnitude. Once we have the absolute and apparent magnitude, we apply the distance modulus formula to find the physical distance. v Supemova v Hubble's Law D. Measuring distance by measuring the length of time that it takes for radiation to reflect off of a target and return to a detector on Earth. That time is then divided by 2 and multiplied by the speed of light to get the one-way distance. E. We measure the recessional velocities of galaxies and divide that speed by the rate at which the space between galaxies expands per megaparsec to determine the number of megaparsecs between own galaxy and the one we observed. F. The process of measuring the absolute magnitudes of a cluster of stars by aligning them with a portion of the H-R diagram and then pairing that information with their apparent magnitudes to work out the distance modulus and physical distance to the stars. G. Done by fitting a star's spectrum to that of similar stars on the H-R diagram. Doing so provides the star's expected absolute magnitude which, when paired with the star's observed apparent magnitude, allows the observer to apply the distance modulus formula to gather the physical distance to the star.
Transcribed Image Text:QUESTION 19 Match the following techniques for determining the distances to astronomical bodies to the descriptions: v Radar Ranging A. Uses shifting perspective to measure how the foreground objects shift relative to objects in the background. The effects are more noticeable the longer the baseline between the two observation points (i.e. moving from one side of the Sun to the other) v Trigonometric Parallax v Spectroscopic Parallax B. The process or relying on a relation between a star's period of pulsation and its overall luminosity to provide its absolute magnitude, which then can be paired with the observed apparent magnitude to work out the distance modulus and physical distance to the star. v Main sequence fitting v Variable Stars C. The process of fitting an observed variation in brightness as the light of this standard candle dims over time to models that can provide the event's absolute magnitude. Once we have the absolute and apparent magnitude, we apply the distance modulus formula to find the physical distance. v Supemova v Hubble's Law D. Measuring distance by measuring the length of time that it takes for radiation to reflect off of a target and return to a detector on Earth. That time is then divided by 2 and multiplied by the speed of light to get the one-way distance. E. We measure the recessional velocities of galaxies and divide that speed by the rate at which the space between galaxies expands per megaparsec to determine the number of megaparsecs between own galaxy and the one we observed. F. The process of measuring the absolute magnitudes of a cluster of stars by aligning them with a portion of the H-R diagram and then pairing that information with their apparent magnitudes to work out the distance modulus and physical distance to the stars. G. Done by fitting a star's spectrum to that of similar stars on the H-R diagram. Doing so provides the star's expected absolute magnitude which, when paired with the star's observed apparent magnitude, allows the observer to apply the distance modulus formula to gather the physical distance to the star.
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