Hot Spots Drift in Synchronous and Asynchronous Polars: Results of Three-Dimensional Numerical Simulation
In this paper, the characteristics of hot spots on an accretor surface are investigated for two types of polars: the eclipsing synchronous polar V808 Aur and the non-eclipsing asynchronous polar CD Ind in configuration of an offset and non-offset magnetic dipole. The drift of hot spots is analyzed b...
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MDPI AG
2021-11-01
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| Online Access: | https://www.mdpi.com/2075-4434/9/4/110 |
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| author | Dmitry Bisikalo Andrey Sobolev Andrey Zhilkin |
| author_facet | Dmitry Bisikalo Andrey Sobolev Andrey Zhilkin |
| author_sort | Dmitry Bisikalo |
| collection | DOAJ |
| description | In this paper, the characteristics of hot spots on an accretor surface are investigated for two types of polars: the eclipsing synchronous polar V808 Aur and the non-eclipsing asynchronous polar CD Ind in configuration of an offset and non-offset magnetic dipole. The drift of hot spots is analyzed based on the results of numerical calculations and maps of the temperature distribution over the accretor surface. It is shown that a noticeable displacement of the spots is determined by the ratio of ballistic and magnetic parts of the jet trajectory. In the synchronous polar, the dominant influence on the drift of hot spots is exerted by variations in the mass transfer rate, which entail a change in the ballistic part of the trajectory. It was found that when the mass transfer rate changes within the range of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msup><mn>10</mn><mrow><mo>−</mo><mn>10</mn></mrow></msup><msub><mi>M</mi><mo>⊙</mo></msub><mo>/</mo><mi>year</mi></mrow></semantics></math></inline-formula> to <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msup><mn>10</mn><mrow><mo>−</mo><mn>7</mn></mrow></msup><msub><mi>M</mi><mo>⊙</mo></msub><mo>/</mo><mi>year</mi></mrow></semantics></math></inline-formula>, the displacement of the hot spot in latitude and longitude can reach <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>30</mn><mo>∘</mo></msup></semantics></math></inline-formula>. In the asynchronous polar, a change in the position of hot spots is mainly defined by the properties of the white dwarf magnetosphere, and the displacement of hot spots in latitude and longitude can reach <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>20</mn><mo>∘</mo></msup></semantics></math></inline-formula>. |
| first_indexed | 2024-03-10T04:03:56Z |
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| id | doaj.art-0648c46b4c394655a6ae4e9d34ea6500 |
| institution | Directory Open Access Journal |
| issn | 2075-4434 |
| language | English |
| last_indexed | 2024-03-10T04:03:56Z |
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| spelling | doaj.art-0648c46b4c394655a6ae4e9d34ea65002023-11-23T08:26:21ZengMDPI AGGalaxies2075-44342021-11-019411010.3390/galaxies9040110Hot Spots Drift in Synchronous and Asynchronous Polars: Results of Three-Dimensional Numerical SimulationDmitry Bisikalo0Andrey Sobolev1Andrey Zhilkin2Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya St., 119017 Moscow, RussiaInstitute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya St., 119017 Moscow, RussiaInstitute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya St., 119017 Moscow, RussiaIn this paper, the characteristics of hot spots on an accretor surface are investigated for two types of polars: the eclipsing synchronous polar V808 Aur and the non-eclipsing asynchronous polar CD Ind in configuration of an offset and non-offset magnetic dipole. The drift of hot spots is analyzed based on the results of numerical calculations and maps of the temperature distribution over the accretor surface. It is shown that a noticeable displacement of the spots is determined by the ratio of ballistic and magnetic parts of the jet trajectory. In the synchronous polar, the dominant influence on the drift of hot spots is exerted by variations in the mass transfer rate, which entail a change in the ballistic part of the trajectory. It was found that when the mass transfer rate changes within the range of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msup><mn>10</mn><mrow><mo>−</mo><mn>10</mn></mrow></msup><msub><mi>M</mi><mo>⊙</mo></msub><mo>/</mo><mi>year</mi></mrow></semantics></math></inline-formula> to <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msup><mn>10</mn><mrow><mo>−</mo><mn>7</mn></mrow></msup><msub><mi>M</mi><mo>⊙</mo></msub><mo>/</mo><mi>year</mi></mrow></semantics></math></inline-formula>, the displacement of the hot spot in latitude and longitude can reach <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>30</mn><mo>∘</mo></msup></semantics></math></inline-formula>. In the asynchronous polar, a change in the position of hot spots is mainly defined by the properties of the white dwarf magnetosphere, and the displacement of hot spots in latitude and longitude can reach <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>20</mn><mo>∘</mo></msup></semantics></math></inline-formula>.https://www.mdpi.com/2075-4434/9/4/110close binary starpolarMHDflow structuredonoraccretor |
| spellingShingle | Dmitry Bisikalo Andrey Sobolev Andrey Zhilkin Hot Spots Drift in Synchronous and Asynchronous Polars: Results of Three-Dimensional Numerical Simulation Galaxies close binary star polar MHD flow structure donor accretor |
| title | Hot Spots Drift in Synchronous and Asynchronous Polars: Results of Three-Dimensional Numerical Simulation |
| title_full | Hot Spots Drift in Synchronous and Asynchronous Polars: Results of Three-Dimensional Numerical Simulation |
| title_fullStr | Hot Spots Drift in Synchronous and Asynchronous Polars: Results of Three-Dimensional Numerical Simulation |
| title_full_unstemmed | Hot Spots Drift in Synchronous and Asynchronous Polars: Results of Three-Dimensional Numerical Simulation |
| title_short | Hot Spots Drift in Synchronous and Asynchronous Polars: Results of Three-Dimensional Numerical Simulation |
| title_sort | hot spots drift in synchronous and asynchronous polars results of three dimensional numerical simulation |
| topic | close binary star polar MHD flow structure donor accretor |
| url | https://www.mdpi.com/2075-4434/9/4/110 |
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