Radiation-Driven Wind Hydrodynamics of Massive Stars: A Review
Mass loss from massive stars plays a determining role in their evolution through the upper Hertzsprung–Russell diagram. The hydrodynamic theory that describes their steady-state winds is the line-driven wind theory (m-CAK). From this theory, the mass loss rate and the velocity profile of the wind ca...
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| Format: | Article |
| Language: | English |
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MDPI AG
2023-05-01
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| Series: | Galaxies |
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| Online Access: | https://www.mdpi.com/2075-4434/11/3/68 |
| _version_ | 1797594727449624576 |
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| author | Michel Curé Ignacio Araya |
| author_facet | Michel Curé Ignacio Araya |
| author_sort | Michel Curé |
| collection | DOAJ |
| description | Mass loss from massive stars plays a determining role in their evolution through the upper Hertzsprung–Russell diagram. The hydrodynamic theory that describes their steady-state winds is the line-driven wind theory (m-CAK). From this theory, the mass loss rate and the velocity profile of the wind can be derived, and estimating these properly will have a profound impact on quantitative spectroscopy analyses from the spectra of these objects. Currently, the so-called <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>β</mi></semantics></math></inline-formula> law, which is an approximation for the fast solution, is widely used instead of m-CAK hydrodynamics, and when the derived value is <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>β</mi><mo>≳</mo><mn>1.2</mn></mrow></semantics></math></inline-formula>, there is no hydrodynamic justification for these values. This review focuses on (1) a detailed topological analysis of the equation of motion (EoM), (2) solving the EoM numerically for all three different (fast and two slow) wind solutions, (3) deriving analytical approximations for the velocity profile via the Lambert<i>W</i> function and (4) presenting a discussion of the applicability of the slow solutions. |
| first_indexed | 2024-03-11T02:26:18Z |
| format | Article |
| id | doaj.art-4faaa392793e440e8c3aef966dc023d8 |
| institution | Directory Open Access Journal |
| issn | 2075-4434 |
| language | English |
| last_indexed | 2024-03-11T02:26:18Z |
| publishDate | 2023-05-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Galaxies |
| spelling | doaj.art-4faaa392793e440e8c3aef966dc023d82023-11-18T10:31:12ZengMDPI AGGalaxies2075-44342023-05-011136810.3390/galaxies11030068Radiation-Driven Wind Hydrodynamics of Massive Stars: A ReviewMichel Curé0Ignacio Araya1Instituto de Física y Astronomía, Universidad de Valparaíso, Gran Bretaña 1111, Valparaíso 2340000, ChileVicerrectoría de Investigación, Universidad Mayor, Santiago 8580745, ChileMass loss from massive stars plays a determining role in their evolution through the upper Hertzsprung–Russell diagram. The hydrodynamic theory that describes their steady-state winds is the line-driven wind theory (m-CAK). From this theory, the mass loss rate and the velocity profile of the wind can be derived, and estimating these properly will have a profound impact on quantitative spectroscopy analyses from the spectra of these objects. Currently, the so-called <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>β</mi></semantics></math></inline-formula> law, which is an approximation for the fast solution, is widely used instead of m-CAK hydrodynamics, and when the derived value is <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>β</mi><mo>≳</mo><mn>1.2</mn></mrow></semantics></math></inline-formula>, there is no hydrodynamic justification for these values. This review focuses on (1) a detailed topological analysis of the equation of motion (EoM), (2) solving the EoM numerically for all three different (fast and two slow) wind solutions, (3) deriving analytical approximations for the velocity profile via the Lambert<i>W</i> function and (4) presenting a discussion of the applicability of the slow solutions.https://www.mdpi.com/2075-4434/11/3/68stars: massivestars: mass-losshydrodynamicsanalytical methodsnumerical methods |
| spellingShingle | Michel Curé Ignacio Araya Radiation-Driven Wind Hydrodynamics of Massive Stars: A Review Galaxies stars: massive stars: mass-loss hydrodynamics analytical methods numerical methods |
| title | Radiation-Driven Wind Hydrodynamics of Massive Stars: A Review |
| title_full | Radiation-Driven Wind Hydrodynamics of Massive Stars: A Review |
| title_fullStr | Radiation-Driven Wind Hydrodynamics of Massive Stars: A Review |
| title_full_unstemmed | Radiation-Driven Wind Hydrodynamics of Massive Stars: A Review |
| title_short | Radiation-Driven Wind Hydrodynamics of Massive Stars: A Review |
| title_sort | radiation driven wind hydrodynamics of massive stars a review |
| topic | stars: massive stars: mass-loss hydrodynamics analytical methods numerical methods |
| url | https://www.mdpi.com/2075-4434/11/3/68 |
| work_keys_str_mv | AT michelcure radiationdrivenwindhydrodynamicsofmassivestarsareview AT ignacioaraya radiationdrivenwindhydrodynamicsofmassivestarsareview |