Zobrazeno 1 - 10
of 25
pro vyhledávání: '"Ootes, L. S."'
Transient LMXBs that host neutron stars (NSs) provide excellent laboratories for probing the dense matter physics present in NS crusts. During accretion outbursts in LMXBs, exothermic reactions may heat the NS crust, disrupting the crust-core equilib
Externí odkaz:
http://arxiv.org/abs/2005.12014
Autor:
Degenaar, N., Ootes, L. S., Page, D., Wijnands, R., Parikh, A. S., Homan, J., Cackett, E. M., Miller, J. M., Altamirano, D., Linares, M.
The structure and composition of the crust of neutron stars plays an important role in their thermal and magnetic evolution, hence in setting their observational properties. One way to study the crust properties is to measure how it cools after it ha
Externí odkaz:
http://arxiv.org/abs/1907.07205
Recurrent low-level luminosity behaviour after a giant outburst in the Be/X-ray transient 4U 0115+63
Autor:
Escorial, A. Rouco, Wijnands, R., Eijnden, J. van den, Patruno, A., Degenaar, N., Parikh, A., Ootes, L. S.
Publikováno v:
A&A 638, A152 (2020)
In 2017, the Be/X-ray transient 4U 0115+63 exhibited a new type-II outburst that was two times fainter than its 2015 giant outburst (in the Swift/BAT count rates). Despite this difference between the two bright events, the source displayed similar X-
Externí odkaz:
http://arxiv.org/abs/1907.04724
Publikováno v:
A&A 630, A95 (2019)
Transient neutron star (NS) LMXBs undergo episodes of accretion, alternated with quiescent periods. During an accretion outburst, the NS heats up due to exothermic accretion-induced processes taking place in the crust. Besides the long-known deep cru
Externí odkaz:
http://arxiv.org/abs/1906.02554
Autor:
Parikh, A. S., Wijnands, R., Ootes, L. S., Page, D., Degenaar, N., Bahramian, A., Brown, E. F., Cackett, E. M., Cumming, A., Heinke, C., Homan, J., Escorial, A. Rouco, Wijngaarden, M. J. P.
Publikováno v:
A&A 624, A84 (2019)
Monitoring the cooling of neutron-star crusts heated during accretion outbursts allows us to infer the physics of the dense matter present in the crust. We examine the crust cooling evolution of the low-mass X-ray binary MXB 1659-29 up to ~505 days a
Externí odkaz:
http://arxiv.org/abs/1810.05626
Autor:
Escorial, A. Rouco, Wijnands, R., Ootes, L. S., Degenaar, N., Snelders, M., Kaper, L., Cackett, E. M., Homan, J.
Publikováno v:
A&A 630, A105 (2019)
The Be/X-ray transient GRO J1750-27 exhibited a type-II (giant) outburst in 2015. After the source transited to quiescence, we triggered our multi-year Chandra monitoring programme to study its quiescent behaviour. The programme was designed to follo
Externí odkaz:
http://arxiv.org/abs/1809.10264
Autor:
Ootes, L. S., Vats, S., Page, D., Wijnands, R., Parikh, A. S., Degenaar, N., Wijngaarden, M. J. P., Altamirano, D., Bahramian, A., Cackett, E. M., Heinke, C. O., Homan, J., Miller, J. M.
We present a new Chandra observation (performed in July 2016) of the neutron star X-ray transient IGR J17480-2446, located in the globular cluster Terzan 5. We study the continued cooling of the neutron star crust in this system that was heated durin
Externí odkaz:
http://arxiv.org/abs/1805.00610
In accreting neutron star X-ray transients, the neutron star crust can be substantially heated out of thermal equilibrium with the core during an accretion outburst. The observed subsequent cooling in quiescence (when accretion has halted) offers a u
Externí odkaz:
http://arxiv.org/abs/1712.02272
Autor:
Parikh, A. S., Homan, J., Wijnands, R., Ootes, L. S., Page, D., Degenaar, D. Altamirano. N., Brown, E. F., Cackett, E. M., Cumming, A., Deibel, A., Fridriksson, J. K., Lin, D., Linares, M., Miller, J. M.
The transient neutron star (NS) low-mass X-ray binary MAXI J0556$-$332 provides a rare opportunity to study NS crust heating and subsequent cooling for multiple outbursts of the same source. We examine {\it MAXI}, {\it Swift}, {\it Chandra}, and {\it
Externí odkaz:
http://arxiv.org/abs/1710.09365
The neutron star low-mass X-ray binary and intermittent millisecond X-ray pulsar HETE J1900.1-2455 returned to quiescence in late 2015, after a prolonged accretion outburst of ~10 yr. Using a Chandra observation taken ~180 d into quiescence we detect
Externí odkaz:
http://arxiv.org/abs/1609.07485