# Young pre-Low-Mass X-ray Binaries in propeller phase : Nature of the 6.7-hour periodic X-ray source 1E 161348-5055 in RCW 103

## TL;DR

This paper proposes a model where a young, fast-spinning neutron star in a pre-Low-Mass X-ray Binary with an eccentric orbit explains the 6.7-hour periodic X-ray emission through orbitally-modulated accretion and propeller mechanisms.

## Contribution

It introduces a detailed model of a pre-LMXB system with a neutron star explaining the observed periodicity and spectral properties, aligning with standard formation theories.

## Key findings

- Model reproduces the 6.7-hour X-ray periodicity.
- Spectral properties match observational data.
- System evolution consistent with standard theories.

## Abstract

Discovery of the 6.7-hour periodicity in the X-ray source 1E 161348-5055 in RCW 103 has led to investigations of the nature of this periodicity. We explore a model for 1E 161348-5055, wherein a fast-spinning neutron star with a magnetic field $\sim 10^{12}$ G in a young pre-Low-Mass X-ray Binary (pre-LMXB) with an eccentric orbit of period 6.7 hr operates in the "propeller" phase. The 6.7-hr light curve of 1E 161348-5055 can be quantitatively accounted by a model of orbitally-modulated mass transfer through a viscous accretion disk and subsequent propeller emission (both Illarionov-Sunyaev type and Romanova-Lovelace et al type), and spectral and other properties are also in agreement. Formation and evolution of model systems are shown to be in accordance both with standard theories.