SIMBAD references

2020ApJ...896...55G - Astrophys. J., 896, 55-55 (2020/June-2)

Discovery of delayed spin-up behavior following two large glitches in the Crab pulsar, and the statistics of such processes.

GE M.Y., ZHANG S.N., LU F.J., LI T.P., YUAN J.P., ZHENG X.P., HUANG Y., ZHENG S.J., CHEN Y.P., CHANG Z., TUO Y.L., CHENG Q., GUNGOR C., SONG L.M., XU Y.P., CAO X.L., CHEN Y., LIU C.Z., ZHANG S., QU J.L., BU Q.C., CAI C., CHEN G., CHEN L., CHEN M.Z., CHEN T.X., CHEN Y.B., CUI W., CUI W.W., DENG J.K., DONG Y.W., DU Y.Y., FU M.X., GAO G.H., GAO H., GAO M., GU Y.D., GUAN J., GUO C.C., HAN D.W., HAO L.F., HUO J., JIA S.M., JIANG L.H., JIANG W.C., JIN C.J., JIN J., JIN Y.J., KONG L.D., LI B., LI D., LI C.K., LI G., LI M.S., LI W., LI X., LI X.B., LI X.F., LI Y.G., LI Z.W., LI Z.X., LIU Z.Y., LIANG X.H., LIAO J.Y., LIU G.Q., LIU H.W., LIU X.J., LIU Y.N., LU B., LU X.F., LUO Q., LUO T., MA X., MENG B., NANG Y., NIE J.Y., OU G., SAI N., SHANG R.C., SONG X.Y., SUN L., TAN Y., TAO L., WANG C., WANG G.F., WANG J., WANG J.B., WANG M., WANG N., WANG W.S., WANG Y.D., WANG Y.S., WEN X.Y., WEN Z.G., WU B.B., WU B.Y., WU M., XIAO G.C., XIAO S., XIONG S.L., XU Y.H., YAN W.M., YANG J.W., YANG S., YANG Y.J., YANG Y.J., YI Q.B., YIN Q.Q., YOU Y., YUE Y.L., ZHANG A.M., ZHANG C.M., ZHANG D.P., ZHANG F., ZHANG H.M., ZHANG J., ZHANG T., ZHANG W.C., ZHANG W., ZHANG W.Z., ZHANG Y., ZHANG Y.F., ZHANG Y.J., ZHANG Y., ZHANG Z., ZHANG Z., ZHANG Z.L., ZHAO H.S., ZHAO X.F., ZHENG W., ZHOU D.K., ZHOU J.F., ZHOU X., ZHUANG R.L., ZHU Y.X. and ZHU Y.

Abstract (from CDS):

Glitches correspond to sudden jumps of rotation frequency (ν) and its derivative ({dot}ν) of pulsars, the origin of which remains not well understood yet, partly because the jump processes of most glitches are not well time-resolved. There are three large glitches of the Crab pulsar, detected in 1989, 1996, and 2017, which were found to have delayed spin-up processes before the normal recovery processes. Here we report two additional glitches of this pulsar that occurred in 2004 and 2011 for which we discovered delayed spin-up processes, and present refined parameters of the largest glitch, which occurred in 2017. The initial rising time of the glitch is determined as <0.48 hr. The two glitches that occurred in 2004 and 2011 had delayed spin-up time scales (τ1) of 1.7 ± 0.8 days and 1.6 ± 0.4 days, respectively. We also carried out a statistical study of these five glitches with observed spin-up processes. We find that the Δν versus | Δ{dot}ν| relation of these five glitches is similar to those with no detected delayed spin-up process, indicating that they are similar to the others in nature except that they have larger amplitudes. For these five glitches, the amplitudes of the delayed spin-up process (| Δνd1| ) and recovery process (Δνd2), their time scales (τ1, τ2), and permanent changes in spin frequency (Δνp) and total frequency step (Δνg) have positive correlations. From these correlations, we suggest that the delayed spin-up processes are common for all glitches, but are too short and thus difficult to be detected for most glitches.

Abstract Copyright: © 2020. The American Astronomical Society. All rights reserved.

Journal keyword(s): Neutron stars - Rotation powered pulsars - Neutron star cores - Nuclear astrophysics

Simbad objects: 3

goto Full paper

goto View the references in ADS

To bookmark this query, right click on this link: simbad:2020ApJ...896...55G and select 'bookmark this link' or equivalent in the popup menu