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Rapidly Spinning Compact Stars with Deconfinement Phase Transition

  • Authors: Tuna Demircik, Christian Ecker, and Matti Järvinen

2021 The Astrophysical Journal Letters 907 L37.

  • Provider: AAS Journals

Caption: Figure 4.

Mass–radius relations for soft (left panel), intermediate (middle panel) and stiff (right panel) EoS. Red (blue) curves are for non-rotating (maximally rotating) configurations, the red dashed line is the unstable branch in the quark matter phase, and cyan, orange, green, and purple lines are sequences of fixed rotational frequency. The horizontal bands show the result for the mass of the secondary component of GW190814 (light green) and the most stringent bounds on the maximum mass of static NSs (light blue and light red; Cromartie et al. 2019; Most et al. 2020). In addition, we show observational bounds deduced from PSR J0030+0451 by the Neutron star Interior Composition Explorer (NICER; Miller et al. 2019; Riley et al. 2019; pink ellipses) and from the measurement of the X-ray binary 4U 1702-429 (Nättilä et al. 2017; cyan area).

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