Hitomi X-ray studies of giant radio pulses from the Crab pulsar

• Authors: AHARONIAN F.; AKAMATSU H.; AKIMOTO F.; ALLEN SW; ANGELINI L.; AUDARD M.; AWAKI H.; AXELSSON M.; BAMBA A.; BAUTZ MW; BLANDFORD R.; BRENNEMAN LW; BROWN GV; BULBUL E.; CACKETT EM; CHERNYAKOVA M.; CHIAO MP; COPPI PS; COSTANTINI E.; DE PLAA J.; DE VRIES CP; DEN HERDER JW; DONE C.; DOTANI T.; EBISAWA K.; ECKART ME; ENOTO T.; EZOE Y.; FABIAN AC; FERRIGNO C.; FOSTER AR; FUJIMOTO R.; FUKAZAWA Y.; FURUZAWA A.; GALEAZZI M.; GALLO LC; GANDHI P.; GIUSTINI M.; GOLDWURM A.; LY Gu; GUAINAZZI M.; HABA Y.; HAGINO K.; HAMAGUCHI K.; HARRUS IM; HATSUKADE I.; HAYASHI K.; HAYASHI T.; HAYASHIDA K.; HIRAGA JS; HORNSCHEMEIER A.; HOSHINO A.; HUGHES JP; ICHINOHE Y.; IIZUKA R.; INOUE H.; INOUE Y.; ISHIDA M.; ISHIKAWA K.; ISHISAKI Y.; IWAI M.; KAASTRA J.; KALLMAN T.; KAMAE T.; KATAOKA J.; KATSUDA S.; KAWAI N.; KELLEY RL; KILBOURNE CA; KITAGUCHI T.; KITAMOTO S.; KITAYAMA T.; KOHMURA T.; KOKUBUN M.; KOYAMA K.; KOYAMA S.; KRETSCHMAR P.; KRIMM HA; KUBOTA A.; KUNIEDA H.; LAURENT P.; LEE SH; LEUTENEGGER MA; LIMOUSIN OO; LOEWENSTEIN M.; LONG KS; LUMB D.; MADEJSKI G.; MAEDA Y.; MAIER D.; MAKISHIMA K.; MARKEVITCH M.; MATSUMOTO H.; MATSUSHITA K.; MCCAMMON D.; MCNAMARA BR; MEHDIPOUR M.; MILLER ED; MILLER JM; MINESHIGE S.; MITSUDA K.; MITSUISHI I.; MIYAZAWA T.; MIZUNO T.; MORI H.; MORI K.; MUKAI K.; MURAKAMI H.; MUSHOTZKY RF; NAKAGAWA T.; NAKAJIMA H.; NAKAMORI T.; NAKASHIMA S.; NAKAZAWA K.; NOBUKAWA KK; NOBUKAWA M.; NODA H.; ODAKA H.; OHASHI T.; OHNO M.; OKAJIMA T.; OSHIMIZU K.; OTA N.; OZAKI M.; PAERELS F.; PALTANI S.; PETRE R.; PINTO C.; PORTER FS; POTTSCHMIDT K.; REYNOLDS CS; SAFI-HARB S.; SAITO S.; SAKAI K.; SASAKI T.; SATO G.; SATO K.; SATO R.; SAWADA M.; SCHARTEL N.; SERLEMTSOS PJ; SETA H.; SHIDATSU M.; SIMIONESCU A.; SMITH RK; SOONG Y.; STAWARZ L.; SUGAWARA Y.; SUGITA S.; SZYMKOWIAK A.; TAJIMA H.; TAKAHASHI H.; TAKAHASHI T.; TAKEDA S.; TAKEI Y.; TAMAGAWA T.; TAMURA T.; TANAKA T.; TANAKA Y.; TANAKA YT; TASHIRO MS; TAWARA Y.; TERADA Y.; TERASHIMA Y.; TOMBESI F.; TOMIDA H.; TSUBOI Y.; TSUJIMOTO M.; TSUNEMI H.; TSURU TG; UCHIDA H.; UCHIYAMA H.; UCHIYAMA Y.; UEDA S.; UEDA Y.; UNO S.; URRY CM; URSINO E.; WATANABE S.; WERNER Norbert; WILKINS DR; WILLIAMS BJ; YAMADA S.; YAMAGUCHI H.; YAMAOKA K.; YAMASAKI NY; YAMAUCHI M.; YAMAUCHI S.; YAQOOB T.; YATSU Y.; YONETOKU D.; ZHURAVLEVA I.; ZOGHBI A.; TERASAWA T.; SEKIDO M.; TAKEFUJI K.; KAWAI E.; MISAWA H.; TSUCHIYA F.; YAMAZAKI R.; KOBAYASHI E.; KISAKA S.; AOKI T.
• Year of publication: 2018
• Type: Article in Periodical
• Magazine / Source: PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
• MU Faculty or unit: Faculty of Science

Web

• https://academic.oup.com/pasj/article/70/2/15/4969720
• https://ui.adsabs.harvard.edu/abs/2018PASJ...70...15H/abstract

• Doi: http://dx.doi.org/10.1093/pasj/psx083
• Keywords: pulsars: individual (B0531+21); radio continuum: stars; X-rays: stars
• Description: To search for giant X-ray pulses correlated with the giant radio pulses (GRPs) from the Crab pulsar, we performed a simultaneous observation of the Crab pulsar with the X-ray satellite Hitomi in the 2-300 keV band and the Kashima NICT radio telescope in the 1.4-1.7 GHz band with a net exposure of about 2 ks on 2016 March 25, just before the loss of the Hitomi mission. The timing performance of the Hitomi instruments was confirmed to meet the timing requirement and about 1000 and 100 GRPs were simultaneously observed at the main pulse and inter-pulse phases, respectively, and we found no apparent correlation between the giant radio pulses and the X-ray emission in either the main pulse or inter-pulse phase. All variations are within the 2 sigma fluctuations of the X-ray fluxes at the pulse peaks, and the 3 sigma upper limits of variations of main pulse or inter-pulse GRPs are 22% or 80% of the peak flux in a 0.20 phase width, respectively, in the 2-300 keV band. The values for main pulse or inter-pulse GRPs become 25% or 110%, respectively, when the phase width is restricted to the 0.03 phase. Among the upper limits from the Hitomi satellite, those in the 4.5-10 keV and 70-300 keV bands are obtained for the first time, and those in other bands are consistent with previous reports. Numerically, the upper limits of the main pulse and inter-pulse GRPs in the 0.20 phase width are about (2.4 and 9.3) x 10(-11) erg cm(-2), respectively. No significant variability in pulse profiles implies that the GRPs originated from a local place within the magneto-sphere. Although the number of photon-emitting particles should temporarily increase to account for the brightening of the radio emission, the results do not statistically rule out variations correlated with the GRPs, because the possible X-ray enhancement may appear due to a > 0.02% brightening of the pulse-peak flux under such conditions.