MG14 - Talk detail |
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Participant |
Lyutikov, Maxim | |||||||
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Institution |
Purdue University, Department of Physics - 525 Northwestern Avenue - United States - IN - USA | |||||||
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Session |
BH7-8 |
Accepted |
Yes |
Order |
2 |
Time |
15:00 | 30' |
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Talk |
Oral abstract |
Title |
Hair of astrophysical black holes | |||||
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Abstract |
The "no hair" theorem is not applicable to black holes formed from collapse of a rotating neutron star. Rotating neutron stars can self-produce particles via vacuum breakdown forming a highly conducting plasma magnetosphere such that magnetic field lines are effectively "frozen-in" the star both before and during collapse. In the limit of no resistivity, this introduces a topological constraint which prohibits the magnetic field from sliding off the newly-formed event horizon. As a result, during collapse of a neutron star into a black hole, the latter conserves the magnetic flux. The black hole's magnetosphere subsequently relaxes to the split monopole magnetic field geometry with self-generated currents outside the event horizon. The dissipation of the resulting equatorial current sheet leads to a slow loss of the anchored flux tubes, a process that balds the black hole on long resistive time scales rather than the short light-crossing time scales expected from the vacuum "no-hair" theorem. |
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Pdf file |
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Session |
BN3 |
Accepted |
Yes |
Order |
4 |
Time |
15:45 | 15' |
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Talk |
Oral abstract |
Title |
The Double Pulsar: whence to pulse. | |||||
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Abstract |
The discovery of the binary radio pulsar system, PSR J0737-3039A/B, surpassed most expectations, both theoretical and observational, as a tool to probe general relativity, stellar evolution and pulsar theories. Unexpectedly, the faster pulsar A is eclipsed once per orbit while the slower pulsar B shows orbital-dependent variations of intensity. I will describe a model of eclipses which reproduces the complicated observed light curve down to intricate details. The model provides a quantitative measurement of relativistic spin precession, offers a new test of theories of gravity, and allows one to determine the location where the enigmatic pulsar radio emission is generated within the magnetosphere. |
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Pdf file |
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Session |
NS5 |
Accepted |
Yes |
Order |
4 |
Time |
16:30 | 25' + 5' |
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Talk |
Oral abstract |
Title |
"Solar flare" model of magnetar activity | |||||
| Coauthors | ||||||||
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Abstract |
We advance a "Solar flare" model of magnetar activity, whereas slow evolution of the magnetic field in the upper crust twists the external magnetic flux tubes, producing persistent emission, bursts and flares. At the same time the neutron star's crust plastically relieves the magnetically imposed strain. Bursts and flares are magnetospheric reconnection events, occurring when the twist of the magnetic field in the magnetosphere exceed a critical value. |
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Pdf file |
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