English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The neutron star low-mass X-ray binary and intermittent millisecond X-raypulsar HETE J1900.1-2455 returned to quiescence in late 2015, after a prolongedaccretion outburst of ~10 yr. Using a Chandra observation taken ~180 d intoquiescence we detect the source at a luminosity of ~4.5E31 (D/4.7 kpc)^2 erg/s(0.5-10 keV). The X-ray spectrum can be described by a neutron star atmospheremodel with a temperature of ~54 eV for an observer at infinity. We performthermal evolution calculations based on the 2016 quiescent data and a <98 eVtemperature upper limit inferred from a Swift observation taken during anunusually brief (<2 weeks) quiescent episode in 2007. We find no evidence inthe present data that the thermal properties of the crust, such as the heatingrate and thermal conductivity, are different than those of non-pulsatingneutron stars. Finding this neutron star so cold after its long outburstimposes interesting constraints on the heat capacity of the stellar core; thesebecome even stronger if further cooling were to occur.

A cold neutron star in the transient low-mass X-ray binary HETE J1900.1-2455 after 10 years of active accretion