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2013), eXTP of the China National Space Administration (CNSA Zhang et al. For example, computing accurate pulse profiles of hot spots on spinning neutron stars has recently been intensively investigated, motivated by many upcoming or planned new space-borne X-ray observatories like ESA’s XIPE ( Soffitta et al. Current and future observations, on the other hand, demand highly accurate models. By introducing BENDER 1, we aim to provide a similar publicly available platform for ray tracing problems focused on spinning compact objects.įollowing the path of photons in a space-time of a rotating neutron star is a challenging task, both theoretically and numerically. Here we instead focus on the emission from rotating neutron stars, for which the Kerr metric is not a good appro- ximation if the star is rotating rapidly.

2016), and GRTRANS ( Dexter 2016), to name a few. 2013), PANDURATA ( Schnittman & Krolik 2013), ASTRORAY ( Shcherbakov & McKinney 2013), HEROIC ( Narayan et al. Existing convenient and modern frameworks for the emission around rotating (typically Kerr) black holes include GEOKERR ( Dexter & Agol 2009), GYOTO ( Vincent et al. Not only is the object curving the space-time around it and hence affecting the trajectory of photons, but it can also affect the apparent observed radiation as the emitting surface can move with relativistic velocities. Key words: methods: numerical / radiative transfer / stars: neutron / gravitationĪccurate modeling of the emission from and around compact objects is a complicated combination of radiative processes and relativity. These allow us to quantify the strength of the pulse fractions one expects to observe from typical fast-spinning millisecond pulsars. We also calculate accurate pulse profiles and observer skymaps of emission from hot spots on rapidly rotating accreting millisecond pulsars. These can then be used to quantitatively estimate the effects of rotational smearing on the observed spectra.

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The full width at tenth-maximum and full width at half-maximum of the rotation smearing kernels are also reported for all viewing angles.

We find that in this metric description, the second-order quadrupole effects are not strong enough to produce narrow observable features in the spectral energy distribution for almost any physically realistic parameter combination, and hence, actually detecting them is unlikely. As an application, we study spectral line profiles (i.e., smearing kernels) from rapidly rotating oblate neutron stars. We also give detailed descriptions of the numerical algorithms used and provide an open-source implementation of the numerical framework called BENDER. We use the Butterworth–Ipser metric expanded up to the second order in rotation and hence include effects of light bending, frame-dragging, and quadrupole deviations on our geodesic calculations. Using a Hamilton-Jacobi formalism, we show that special relativistic rotational effects such as aberration of angles, Doppler boosting, and time dilatation naturally emerge from the general relativistic treatment of rotating compact objects. Nordita, KTH Royal Institute of Technology and Stockholm University,Į-mail: of Helsinki, Department of Physics,Ī theoretical framework for emission originating from rapidly rotating oblate compact objects is described in detail. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes

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