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Nuclear Theory·nucl-th

Monday·July 6, 2020

8 papers—5 primary·3 cross-listed

All8Primary5Cross-lists3
  1. 06

    An attractive spin-orbit potential from the Skyrme model

    Chris Halcrow🇬🇧 · Derek Harland🇬🇧

    We derive the nucleon-nucleon isoscalar spin-orbit potential from the Skyrme model and find good agreement with the Paris potential. This solves a problem that has been open for more than thirty years and gives a new geometric understanding of the spin-orbit force. Our calculation is based on the dipole approximation to skyrmion dynamics and higher order perturbation theory.

    ↳ hep-thnucl-thPRL(2020)·15 citations
  2. 07

    Color Glass Condensate at next-to-leading order meets HERA data

    G. Beuf🇫🇮 · H. Hänninen🇫🇮 · T. Lappi🇫🇮 · H. Mäntysaari🇫🇮

    We perform the first dipole picture fit to HERA inclusive cross section data using the full next-to-leading order (NLO) impact factor combined with an improved Balitsky-Kovchegov evolution including the dominant effects beyond leading logarithmic accuracy at low . We find that three different formulations of the evolution equation that have been proposed in the recent literature result in a very similar description of HERA data, and robust predictions for future deep inelastic scattering experiments. We find evidence pointing towards a significant nonperturbative contribution to the structure function for light quarks, which stresses the need to extend the NLO impact factor calculation to massive quarks.

    ↳ hep-phnucl-thPRD(2020)·111 citations
  3. 08

    Experimental constraints on shallow heating in accreting neutron-star crusts

    Nicolas Chamel🇧🇪 · Anthea Francesca Fantina🇫🇷 · Julian-Leszek Zdunik🇵🇱 · Pawel Haensel🇵🇱

    The observed thermal relaxation of transiently accreting neutron stars during quiescence periods in low-mass X-ray binaries suggests the existence of unknown heat sources in the shallow layers of neutron-star crust. Making use of existing experimental nuclear data, we estimate the maximum possible amount of heat that can be deposited in the outer crust of an accreting neutron star due to electron captures and pycnonuclear fusion reactions triggered by the burial of X-ray burst ashes.

    ↳ astro-ph.HEnucl-thPRC(2020)·22 citations

Affiliations

first authorsco-authorsvia INSPIRE