Figure 2 from Constraining the Neutron Star Mass–Radius Relation and Dense Matter Equation of State with NICER. II. Emission from Hot Spots on a Rapidly Rotating Neutron Star

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Constraining the Neutron Star Mass–Radius Relation and Dense Matter Equation of State with NICER. II. Emission from Hot Spots on a Rapidly Rotating Neutron Star

Authors: Slavko Bogdanov, Frederick K. Lamb, Simin Mahmoodifar, M. Coleman Miller, Sharon M. Morsink, Thomas E. Riley, Tod E. Strohmayer, Albert K. Tung, Anna L. Watts, Alexander J. Dittmann, Deepto Chakrabarty, Sebastien Guillot, Zaven Arzoumanian, and Keith C. Gendreau

2019 The Astrophysical Journal Letters 887 L26.

Provider: AAS Journals

Caption: Figure 2.

Comparison of flux measured at 1 keV for the S+D and OS approximations and the exact numerical waveform for one sample star. The example star spins with a frequency of 200 Hz, has M = 1.44 M_⊙, R_eq = 11.41 km. The upper panel shows waveforms computed using the S+D and OS approximations, as well as the exact numerical waveform. The lower panel shows the percent difference between the approximate and exact solutions.

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