Matches in SemOpenAlex for { <https://semopenalex.org/work/W4311739936> ?p ?o ?g. }
- W4311739936 endingPage "5176" @default.
- W4311739936 startingPage "5161" @default.
- W4311739936 abstract "ABSTRACT Pulsars are rotating neutron stars that emit periodic electromagnetic radiation. While pulsars generally slow down as they lose energy, some also experience glitches: spontaneous increases of their rotational frequency. According to several models, these glitches can also lead to the emission of long-duration transient gravitational waves (GWs). We present detection prospects for such signals by comparing indirect energy upper limits on GW strain for known glitches with the sensitivity of current and future ground-based GW detectors. We first consider the optimistic case of generic constraints based on the glitch size and find that realistic matched-filter searches in the fourth LIGO–Virgo–KAGRA observing run (O4) could make a detection, or set constraints below these indirect upper limits, for equivalents of 36 out of 726 previously observed glitches, and 74 in the O5 run. With the third-generation Einstein Telescope or Cosmic Explorer, 35–40 per cent of glitches would be accessible. When specializing to a scenario where transient mountains produce the post-glitch GW emission, following the Yim & Jones model, the indirect upper limits are stricter. Out of the smaller set of 119 glitches with measured healing parameter, as needed for predictions under that model, only 6 glitches would have been within reach for O4 and 14 for O5, with a similar percentage as before with third-generation detectors. We also discuss how this model matches the observed glitch population." @default.
- W4311739936 created "2022-12-28" @default.
- W4311739936 creator A5003412615 @default.
- W4311739936 creator A5026041327 @default.
- W4311739936 creator A5050040733 @default.
- W4311739936 creator A5080743909 @default.
- W4311739936 date "2022-12-15" @default.
- W4311739936 modified "2023-10-17" @default.
- W4311739936 title "Prospects for detecting transient quasi-monochromatic gravitational waves from glitching pulsars with current and future detectors" @default.
- W4311739936 cites W1537891594 @default.
- W4311739936 cites W1544935943 @default.
- W4311739936 cites W1970770474 @default.
- W4311739936 cites W1973548823 @default.
- W4311739936 cites W1973820399 @default.
- W4311739936 cites W1974013292 @default.
- W4311739936 cites W1981143042 @default.
- W4311739936 cites W1985938529 @default.
- W4311739936 cites W1991133427 @default.
- W4311739936 cites W1992471555 @default.
- W4311739936 cites W1994870116 @default.
- W4311739936 cites W2032121071 @default.
- W4311739936 cites W2036056653 @default.
- W4311739936 cites W2040194587 @default.
- W4311739936 cites W2042358288 @default.
- W4311739936 cites W2043531458 @default.
- W4311739936 cites W2045694681 @default.
- W4311739936 cites W2048729358 @default.
- W4311739936 cites W2056543278 @default.
- W4311739936 cites W2061083933 @default.
- W4311739936 cites W2068169614 @default.
- W4311739936 cites W2076831772 @default.
- W4311739936 cites W2081545524 @default.
- W4311739936 cites W2087051663 @default.
- W4311739936 cites W2091746569 @default.
- W4311739936 cites W2092026720 @default.
- W4311739936 cites W2103857591 @default.
- W4311739936 cites W2117424975 @default.
- W4311739936 cites W2121998732 @default.
- W4311739936 cites W2124050845 @default.
- W4311739936 cites W2138229400 @default.
- W4311739936 cites W2166676688 @default.
- W4311739936 cites W2168368413 @default.
- W4311739936 cites W2169360401 @default.
- W4311739936 cites W2242029913 @default.
- W4311739936 cites W2277831577 @default.
- W4311739936 cites W2323329379 @default.
- W4311739936 cites W2336862676 @default.
- W4311739936 cites W2398579902 @default.
- W4311739936 cites W2416940725 @default.
- W4311739936 cites W2502015268 @default.
- W4311739936 cites W2605670618 @default.
- W4311739936 cites W2762571791 @default.
- W4311739936 cites W2765794294 @default.
- W4311739936 cites W2794861647 @default.
- W4311739936 cites W2800421856 @default.
- W4311739936 cites W2806022225 @default.
- W4311739936 cites W2887267197 @default.
- W4311739936 cites W2895702508 @default.
- W4311739936 cites W2921814238 @default.
- W4311739936 cites W2926718570 @default.
- W4311739936 cites W2958416285 @default.
- W4311739936 cites W2975828310 @default.
- W4311739936 cites W3006908793 @default.
- W4311739936 cites W3013021119 @default.
- W4311739936 cites W3041045135 @default.
- W4311739936 cites W3082432419 @default.
- W4311739936 cites W3091954596 @default.
- W4311739936 cites W3099177382 @default.
- W4311739936 cites W3100187076 @default.
- W4311739936 cites W3102367855 @default.
- W4311739936 cites W3103075183 @default.
- W4311739936 cites W3103389423 @default.
- W4311739936 cites W3104094773 @default.
- W4311739936 cites W3104470507 @default.
- W4311739936 cites W3104789908 @default.
- W4311739936 cites W3105289950 @default.
- W4311739936 cites W3106112140 @default.
- W4311739936 cites W3117462436 @default.
- W4311739936 cites W3122476984 @default.
- W4311739936 cites W3124332909 @default.
- W4311739936 cites W3137391599 @default.
- W4311739936 cites W3175086528 @default.
- W4311739936 cites W3199743929 @default.
- W4311739936 cites W3209312130 @default.
- W4311739936 cites W3213688178 @default.
- W4311739936 cites W3215820161 @default.
- W4311739936 cites W3215825698 @default.
- W4311739936 cites W3216283614 @default.
- W4311739936 cites W3216907171 @default.
- W4311739936 cites W4213199590 @default.
- W4311739936 cites W4221139509 @default.
- W4311739936 cites W4226256235 @default.
- W4311739936 cites W4234856688 @default.
- W4311739936 cites W4290666152 @default.
- W4311739936 cites W4309908840 @default.
- W4311739936 cites W4310155540 @default.
- W4311739936 cites W4320465021 @default.
- W4311739936 doi "https://doi.org/10.1093/mnras/stac3665" @default.