Multi-Wavelength Investigations of the High Magnetic Field Pulsars J1809-1943, J1847-0130, and J1821-1419
Grade Level at Time of Presentation
Junior
Institution
Morehead State University
KY House District #
99
KY Senate District #
27
Faculty Advisor/ Mentor
Thomas Pannuti; Shanil Virani
Department
Department of Physics, Earth Science and Space Systems Engineering
Abstract
Multi-Wavelength Investigations of the High Magnetic Field Pulsars J1809-1943, J1847-0130, and J1821-1419
Colby Winters
Thomas Pannuti
Department of Physics, Earth Science and Space Systems Engineering
Pulsars are the result of massive stars ending their lives in supernova explosions. These explosions produce expanding shells of material (known as supernova remnants -- SNRs) along with a possible central newborn neutron star. Depending on the conditions within the SNR and the formation of the neutron star, either a high magnetic field radio pulsar or a high-energy anomalous X-ray Pulsar (AXP) may form. This research focused on three high magnetic field radio pulsars -- J1809-1943, J1847-0130, and J1821-1419 -- with the intent of exploring the relationships between these sources and their local environments. These pulsars were chosen because they had similar cataloged features as known radio-emitting AXPs, including long periods (from 1 to 8 seconds) and high period derivatives (from 5x10-13 and 10-10). The Green Bank 20-Meter telescope was used to gather timing parameters and pulse profiles on each pulsar at 1.42 GHz. In addition, archival X-ray data from observatories such as Chandra and XMM-Newton were searched for possible X-ray counterparts for these sources. The derived dispersion measures (DMs) were used to calculate distances to these sources and compare our estimated distances to values determined by other methods, such as neutral hydrogen absorption measured through X-ray observations. Ultimately, this research could help extend knowledge about pulsar properties and add to the current understanding of high energy neutron stars.
Multi-Wavelength Investigations of the High Magnetic Field Pulsars J1809-1943, J1847-0130, and J1821-1419
Multi-Wavelength Investigations of the High Magnetic Field Pulsars J1809-1943, J1847-0130, and J1821-1419
Colby Winters
Thomas Pannuti
Department of Physics, Earth Science and Space Systems Engineering
Pulsars are the result of massive stars ending their lives in supernova explosions. These explosions produce expanding shells of material (known as supernova remnants -- SNRs) along with a possible central newborn neutron star. Depending on the conditions within the SNR and the formation of the neutron star, either a high magnetic field radio pulsar or a high-energy anomalous X-ray Pulsar (AXP) may form. This research focused on three high magnetic field radio pulsars -- J1809-1943, J1847-0130, and J1821-1419 -- with the intent of exploring the relationships between these sources and their local environments. These pulsars were chosen because they had similar cataloged features as known radio-emitting AXPs, including long periods (from 1 to 8 seconds) and high period derivatives (from 5x10-13 and 10-10). The Green Bank 20-Meter telescope was used to gather timing parameters and pulse profiles on each pulsar at 1.42 GHz. In addition, archival X-ray data from observatories such as Chandra and XMM-Newton were searched for possible X-ray counterparts for these sources. The derived dispersion measures (DMs) were used to calculate distances to these sources and compare our estimated distances to values determined by other methods, such as neutral hydrogen absorption measured through X-ray observations. Ultimately, this research could help extend knowledge about pulsar properties and add to the current understanding of high energy neutron stars.