no code implementations • 21 Dec 2020 • C. Tiburzi, G. M. Shaifullah, C. G. Bassa, P. Zucca, J. P. W. Verbiest, N. K. Porayko, E. van der Wateren, R. A. Fallows, R. A. Main, G. H. Janssen, J. M. Anderson, A-. S. Bak Nielsen, J. Y. Donner, E. F. Keane, J. Künsemöller, S. Osłowski, J-. M. Grießmeier, M. Serylak, M. Brüggen, B. Ciardi, R. -J. Dettmar, M. Hoeft, M. Kramer, G. Mann, C. Vocks
In a previous paper we studied the Solar-wind (SW) models used in pulsar timing to mitigate the excess of DM annually induced by the SW, and found these to be insufficient for high-precision pulsar timing.
High Energy Astrophysical Phenomena
no code implementations • 15 Dec 2020 • Z. Pleunis, D. Michilli, C. G. Bassa, J. W. T. Hessels, A. Naidu, B. C. Andersen, P. Chawla, E. Fonseca, A. Gopinath, V. M. Kaspi, V. I. Kondratiev, D. Z. Li, M. Bhardwaj, P. J. Boyle, C. Brar, T. Cassanelli, Y. Gupta, A. Josephy, R. Karuppusamy, A. Keimpema, F. Kirsten, C. Leung, B. Marcote, K. Masui, R. Mckinven, B. W. Meyers, C. Ng, K. Nimmo, Z. Paragi, M. Rahman, P. Scholz, K. Shin, K. M. Smith, I. H. Stairs, S. P. Tendulkar
We find that the burst activity is systematically delayed towards lower frequencies by ~3 days from 600 MHz to 150 MHz.
High Energy Astrophysical Phenomena