See Hayashi limit in All languages combined, or Wiktionary
{
"etymology_text": "Named after Japanese astrophysicist Chushiro Hayashi (25 Jul 1920–28 Feb 2010).",
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"examples": [
{
"text": "When a star is fully within hydrostatic equilibrium—a condition where the inward force of gravity is matched by the outward pressure of the gas—the star can not exceed the radius defined by the Hayashi limit.",
"type": "example"
},
{
"ref": "1977, Rudolf Kippenhahn, Walter Strohmeyer, The Interaction of Variable Stars with Their Environment, Remeis-Sternwarte, page 69:",
"text": "However, the approximate locations of the Hayashi limits point to remarkably low masses for the three T Tauri stars investigated here. It should be noted, that the Hayashi limits are valid only for stars in hydrostatic equilibrium.",
"type": "quote"
},
{
"ref": "2006, Peter Eggleton, Evolutionary Processes in Binary and Multiple Stars, Cambridge University Press, page 75:",
"text": "Since the Hayashi limit approaches close to the main sequence at about 1 M⊙, the 'Hertzsprung gap' between the terminal main sequence and the Hayashi limit is much less marked than at high masses.",
"type": "quote"
},
{
"ref": "2009, Donald Gerard Luttermoser, Beverly Joy Smith, Robert E. Stencel, editors, The Biggest, Baddest, Coolest Stars: Proceedings of a Workshop, Astronomical Society of the Pacific, page 33:",
"text": "The latest-type RSGs^([Red Supergiants]) in the Magellanic Clouds are cooler than the current evolutionary tracks allow, occupying the region to the right of the Hayashi limit where stars are no longer in hydrostatic equilibrium.",
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"glosses": [
"A theoretical maximum radius of a star of given mass; the radius at which the inward force of gravity exactly balances the outward pressure of the gas of the star."
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"(astrophysics) A theoretical maximum radius of a star of given mass; the radius at which the inward force of gravity exactly balances the outward pressure of the gas of the star."
],
"related": [
{
"word": "Hayashi boundary"
},
{
"word": "Hayashi track"
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"translations": [
{
"code": "fr",
"lang": "French",
"sense": "theoretical upper limit of the radius of a hydrostatically stable star",
"tags": [
"feminine"
],
"word": "limite de Hayashi"
},
{
"code": "de",
"lang": "German",
"sense": "theoretical upper limit of the radius of a hydrostatically stable star",
"tags": [
"neuter"
],
"word": "Hayashi-Limit"
},
{
"code": "it",
"lang": "Italian",
"sense": "theoretical upper limit of the radius of a hydrostatically stable star",
"tags": [
"masculine"
],
"word": "limite di Hayashi"
}
],
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"Chushiro Hayashi",
"Hayashi limit"
]
}
],
"word": "Hayashi limit"
}
{
"etymology_text": "Named after Japanese astrophysicist Chushiro Hayashi (25 Jul 1920–28 Feb 2010).",
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{
"text": "When a star is fully within hydrostatic equilibrium—a condition where the inward force of gravity is matched by the outward pressure of the gas—the star can not exceed the radius defined by the Hayashi limit.",
"type": "example"
},
{
"ref": "1977, Rudolf Kippenhahn, Walter Strohmeyer, The Interaction of Variable Stars with Their Environment, Remeis-Sternwarte, page 69:",
"text": "However, the approximate locations of the Hayashi limits point to remarkably low masses for the three T Tauri stars investigated here. It should be noted, that the Hayashi limits are valid only for stars in hydrostatic equilibrium.",
"type": "quote"
},
{
"ref": "2006, Peter Eggleton, Evolutionary Processes in Binary and Multiple Stars, Cambridge University Press, page 75:",
"text": "Since the Hayashi limit approaches close to the main sequence at about 1 M⊙, the 'Hertzsprung gap' between the terminal main sequence and the Hayashi limit is much less marked than at high masses.",
"type": "quote"
},
{
"ref": "2009, Donald Gerard Luttermoser, Beverly Joy Smith, Robert E. Stencel, editors, The Biggest, Baddest, Coolest Stars: Proceedings of a Workshop, Astronomical Society of the Pacific, page 33:",
"text": "The latest-type RSGs^([Red Supergiants]) in the Magellanic Clouds are cooler than the current evolutionary tracks allow, occupying the region to the right of the Hayashi limit where stars are no longer in hydrostatic equilibrium.",
"type": "quote"
}
],
"glosses": [
"A theoretical maximum radius of a star of given mass; the radius at which the inward force of gravity exactly balances the outward pressure of the gas of the star."
],
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"(astrophysics) A theoretical maximum radius of a star of given mass; the radius at which the inward force of gravity exactly balances the outward pressure of the gas of the star."
],
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"astrophysics"
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"translations": [
{
"code": "fr",
"lang": "French",
"sense": "theoretical upper limit of the radius of a hydrostatically stable star",
"tags": [
"feminine"
],
"word": "limite de Hayashi"
},
{
"code": "de",
"lang": "German",
"sense": "theoretical upper limit of the radius of a hydrostatically stable star",
"tags": [
"neuter"
],
"word": "Hayashi-Limit"
},
{
"code": "it",
"lang": "Italian",
"sense": "theoretical upper limit of the radius of a hydrostatically stable star",
"tags": [
"masculine"
],
"word": "limite di Hayashi"
}
],
"word": "Hayashi limit"
}
Download raw JSONL data for Hayashi limit meaning in English (3.5kB)
This page is a part of the kaikki.org machine-readable English dictionary. This dictionary is based on structured data extracted on 2024-11-06 from the enwiktionary dump dated 2024-10-02 using wiktextract (fbeafe8 and 7f03c9b). The data shown on this site has been post-processed and various details (e.g., extra categories) removed, some information disambiguated, and additional data merged from other sources. See the raw data download page for the unprocessed wiktextract data.
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