Publications

  • Thermonuclear Bursts with Short Recurrence Times from Neutron Stars Explained by Opacity-Driven Convection. 2017, ApJ 842(2), #113, Keek, L. & Heger, A
  • Dependence of X-ray Burst Models on Nuclear Masses, 2017, accepted by ApJ (arXiv:1610.07596), Hendrik Schatz & Wei-Jia Ong
  • Flux decay during thermonuclear X-ray bursts analysed with the dynamic power-law index method, 2017, accepted by A&A  (arXiv:1705.05653) Kuuttila, J.; Kajava, J. J. E.; Nättilä, J.; Motta, S. E.; Sánchez-Fernández, C.; Kuulkers, E.; Cumming, A.; Poutanen, J.
  • IGR J17062–6143 Is an Accreting Millisecond X-Ray Pulsar, 2017, ApJ Lett. 836, L23, Strohmayer, Tod & Keek, Laurens
  • X-Ray Reflection and an Exceptionally Long Thermonuclear Helium Burst from IGR J17062-6143, 2017, ApJ 836, #111, Keek, L., Iwakiri, W., Serino, M., Ballantyne, D. R., in’t Zand, J. J. M., & Strohmayer, T. E.
  • Thermonuclear Burst Observations for Model Comparisons: A Reference Sample, 2017, PASA 34, e019 (e-print at arXiv:1703.07485, on-line data also at http://burst.sci.monash.edu/reference) Duncan Galloway, Adelle Goodwin, & Laurens Keek
  • Constraints on Bygone Nucleosynthesis from Accreting Neutron Stars, 2017, ApJ 837, #73 (arXiv:1701.02730), Zach Meisel & Alex Deibel
  • Detection of burning ashes from thermonuclear X-ray bursts, 2017, MNRAS 464, L6-10, Kajava, J. J. E.; Nättilä, J.; Poutanen, J.; Cumming, A.; Suleimanov, V.; Kuulkers, E.
  • A Survey of Chemical Separation in Accreting Neutron Stars, 2016, ApJ 823, #117, Mckinven, Ryan; Cumming, Andrew; Medin, Zach; Schatz, Hendrik
  • Accretion Disk Signatures in Type I X-Ray Bursts: Prospects for Future Missions, 2016, ApJ 826, #79, Keek, L., Wolf, Z., & Ballantyne, D. R. 2016
  • Anisotropy of X-Ray Bursts from Neutron Stars with Concave Accretion Disks, 2016, ApJ 819, #47, He, C.-C. & Keek, L.
  • Urca cooling pairs in the neutron star ocean and their effect on superbursts, 2016, ApJ 831, #13 (arXiv:160301281), Alex Deibel, Zach Meisel, Hendrik Schatz, Ed Brown, and Andrew Cumming.