# Constraining the neutron star equation of state using Pulse Profile Modeling

## TL;DR

Pulse Profile Modeling of hotspots on neutron stars, used by NICER and future telescopes, provides a promising method to constrain the dense matter Equation of State by analyzing X-ray emissions.

## Contribution

This paper explains how Pulse Profile Modeling is utilized by NICER and future missions to measure the neutron star Equation of State, highlighting its significance for upcoming X-ray observatories.

## Key findings

- Pulse Profile Modeling effectively constrains neutron star properties.
- NICER's observations demonstrate the technique's potential.
- Future telescopes will enhance EOS measurements.

## Abstract

One very promising technique for measuring the dense matter Equation of State exploits hotspots that form on the neutron star surface due to the pulsar mechanism, accretion streams, or during thermonuclear explosions in the neutron star ocean. This article explains how Pulse Profile Modeling of hotspots is being used by the Neutron Star Interior Composition Explorer (NICER), an X-ray telescope installed on the International Space Station in 2017 - and why the technique is a mission driver for the next, larger-area generation of telescopes including the enhanced X-ray Timing and Polarimetry (eXTP) mission and the Spectroscopic Time-Resolving Observatory for Broadband Energy X-rays (STROBE-X).