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Hub AI
F-type main-sequence star AI simulator
(@F-type main-sequence star_simulator)
Hub AI
F-type main-sequence star AI simulator
(@F-type main-sequence star_simulator)
F-type main-sequence star
An F-type main-sequence star is a main-sequence, core-hydrogen-fusing star of spectral type F. Such stars will generally have a luminosity class of V. They have from around 1.1 to 1.6 times the mass of the Sun and surface temperatures between about 6,000 and 7,200 K. This temperature range gives the F-type stars a whitish hue when observed through the atmosphere.[citation needed] Notable examples include Procyon A, Gamma Virginis A and B, and Tabby's Star.
The revised Yerkes Atlas system (Johnson & Morgan 1953) listed a dense grid of F-type dwarf spectral standard stars; however, not all of these have survived to this day as stable standards.
The anchor points of the MK spectral classification system among the F-type main-sequence dwarf stars, i.e. those standard stars that have remained unchanged over years and can be used to define the system, are considered to be 78 Ursae Majoris (F2 V) and Pi3 Orionis (F6 V). In addition to those two standards, Morgan & Keenan (1973) considered the following stars to be dagger standards: HR 1279 (F3 V), HD 27524 (F5 V), HD 27808 (F8 V), HD 27383 (F9 V), and Beta Virginis (F9 V).
Other primary MK standard stars include HD 23585 (F0 V), HD 26015 (F3 V), and HD 27534 (F5 V). Note that two Hyades members with almost identical HD designations (HD 27524 and HD 27534) are both considered strong F5 V standard stars, and indeed they share nearly identical colors and magnitudes.
Gray & Garrison (1989) provide a modern table of dwarf standards for the hotter F-type stars. F1 and F7 dwarf standards stars are rarely listed, but have changed slightly over the years among expert classifiers. Often-used standard stars in this class include 37 Ursae Majoris (F1 V) and Iota Piscium (F7 V). No F4 V standard stars currently have been officially published.
F9 V defines the boundary between the hot stars classified by Morgan, and the cooler stars classified by Keenan a step lower, and there are discrepancies in the literature on which stars define the F/G dwarf boundary. Morgan & Keenan (1973) listed Beta Virginis and HD 27383 as F9 V standards, but Keenan & McNeil (1989) listed HD 10647 as their F9 V standard instead.
F-type stars have a life-cycle similar to G-type stars. They are hydrogen-fusing and will eventually grow into a red giant once the supply of hydrogen in their cores is depleted. Eventually they shed their outer layers, creating a planetary nebula, and leaving behind, at the center of the nebula, a hot white dwarf.
F-type stars spend 2-6 billion years on the main sequence. In comparison, G-type stars, like the Sun, remain on the main sequence for about 10 billion years.
F-type main-sequence star
An F-type main-sequence star is a main-sequence, core-hydrogen-fusing star of spectral type F. Such stars will generally have a luminosity class of V. They have from around 1.1 to 1.6 times the mass of the Sun and surface temperatures between about 6,000 and 7,200 K. This temperature range gives the F-type stars a whitish hue when observed through the atmosphere.[citation needed] Notable examples include Procyon A, Gamma Virginis A and B, and Tabby's Star.
The revised Yerkes Atlas system (Johnson & Morgan 1953) listed a dense grid of F-type dwarf spectral standard stars; however, not all of these have survived to this day as stable standards.
The anchor points of the MK spectral classification system among the F-type main-sequence dwarf stars, i.e. those standard stars that have remained unchanged over years and can be used to define the system, are considered to be 78 Ursae Majoris (F2 V) and Pi3 Orionis (F6 V). In addition to those two standards, Morgan & Keenan (1973) considered the following stars to be dagger standards: HR 1279 (F3 V), HD 27524 (F5 V), HD 27808 (F8 V), HD 27383 (F9 V), and Beta Virginis (F9 V).
Other primary MK standard stars include HD 23585 (F0 V), HD 26015 (F3 V), and HD 27534 (F5 V). Note that two Hyades members with almost identical HD designations (HD 27524 and HD 27534) are both considered strong F5 V standard stars, and indeed they share nearly identical colors and magnitudes.
Gray & Garrison (1989) provide a modern table of dwarf standards for the hotter F-type stars. F1 and F7 dwarf standards stars are rarely listed, but have changed slightly over the years among expert classifiers. Often-used standard stars in this class include 37 Ursae Majoris (F1 V) and Iota Piscium (F7 V). No F4 V standard stars currently have been officially published.
F9 V defines the boundary between the hot stars classified by Morgan, and the cooler stars classified by Keenan a step lower, and there are discrepancies in the literature on which stars define the F/G dwarf boundary. Morgan & Keenan (1973) listed Beta Virginis and HD 27383 as F9 V standards, but Keenan & McNeil (1989) listed HD 10647 as their F9 V standard instead.
F-type stars have a life-cycle similar to G-type stars. They are hydrogen-fusing and will eventually grow into a red giant once the supply of hydrogen in their cores is depleted. Eventually they shed their outer layers, creating a planetary nebula, and leaving behind, at the center of the nebula, a hot white dwarf.
F-type stars spend 2-6 billion years on the main sequence. In comparison, G-type stars, like the Sun, remain on the main sequence for about 10 billion years.
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