Photoproton decay of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">P</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>31</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>giant resonance

Kerkhove, E.; Ferdinande, H.; Otten, P. Van; Ryckbosch, D.; Vyver, R. Van de; Berkvens, P.; Camp, E. Van; Aksoy, A.

doi:10.1103/physrevc.31.1071

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Proton Production1

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“…where A is the nuclear mass number. Measured crosssections for light elements 10 Z 26 provide evidence for a value xp ≈ 0.5 (Hayward 1963;Kerkhove et al 1985;Assafiri & Thompson 1986). But in the circumstances of shower development below the neutron-star surface, the problem of estimating the effective value of xp is more complicated.…”

Section: Proton Productionmentioning

confidence: 99%

Nuclear physics of reverse electron flow at pulsar polar caps

Jones

2010

Monthly Notices of the Royal Astronomical Society

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Protons produced in electromagnetic showers formed by the reverse-electron flux are usually the largest component of the time-averaged polar-cap open magnetic flux-line current in neutron stars with positive corotational charge density. Although the electric-field boundary conditions in the corotating frame are time-independent, instabilities on both medium and short time-scales cause the current to alternate between states in which either protons or positrons and ions form the major component. These properties are briefly discussed in relation to nulling and microstructure in radio pulsars, pair production in an outer gap, and neutron stars with high surface temperatures.Comment: 13 pages; to be published in Monthly Notices of the Royal Astronomical Societ

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Section: Proton Productionmentioning

confidence: 99%