Estimates of the Surface Magnetic Field Strength of Radio Pulsars
We investigate the geometry of the magnetic field of rotation-powered pulsars. A new method for calculating an angle (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>β</mi></semantics></math&g...
| Main Authors: | , , |
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| Format: | Article |
| Language: | English |
| Published: |
MDPI AG
2023-07-01
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| Series: | Universe |
| Subjects: | |
| Online Access: | https://www.mdpi.com/2218-1997/9/7/334 |
| Summary: | We investigate the geometry of the magnetic field of rotation-powered pulsars. A new method for calculating an angle (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>β</mi></semantics></math></inline-formula>) between the spin and magnetic dipole axes of a neutron star (NS) in the ejector stage is considered within the frame of the magnetic dipole energy loss mechanism. We estimate the surface magnetic field strength (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>B</mi><mi>ns</mi></msub></semantics></math></inline-formula>) for a population of known neutron stars in the radio pulsar (ejector) stage. The evaluated <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi>B</mi><mi>ns</mi></msub><mrow><mo>(</mo><mi>β</mi><mo>)</mo></mrow></mrow></semantics></math></inline-formula> may differ by an order of magnitude from the values without considering the angle <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>β</mi></semantics></math></inline-formula>. It is shown that <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi>B</mi><mi>ns</mi></msub><mrow><mo>(</mo><mi>β</mi><mo>)</mo></mrow></mrow></semantics></math></inline-formula> lies in the range <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>10</mn><mn>8</mn></msup></semantics></math></inline-formula>–<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msup><mn>10</mn><mn>14</mn></msup><mspace width="0.166667em"></mspace><mi mathvariant="normal">G</mi></mrow></semantics></math></inline-formula> for a known population of short and middle periodic radio pulsars. |
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| ISSN: | 2218-1997 |