SoftX-rayemissionpropertiesofMsPs(0.1-10 keV)X-rayemissiondetectedfrom~35MSPs(includingGalactiodisk and globular clusters);Sixofthesehavepulsedemission;Forthree (J0437-4715,J2124-3358,J0030+0451)the emission appearsthermaldominated;Non-thermal emission dominatedfor J0218+4232,B1821-24(inM28),B1937+21.X-ray pulsar windnebulaeof MsPsare also detected27recently (PSR B1957+20,Stappers et al. 2003, Huang et alTwoorigins of PWNe:.Theinteractionbetweenthepulsarwindswiththeinterstellarmedium(isM)-bowshockinteractionbetweenpulsarwindsandthestellarwindsofdonorstars-intrabinaryshock
Soft X-ray emission properties of MSPs (0.1 - 10 keV) • X-ray emission detected from ~35 MSPs (including Galactic disk and globular clusters); • Six of these have pulsed emission; For three (J0437-4715, J2124-3358, J0030+0451) the emission appears thermal dominated; Non-thermal emission dominated for J0218+4232, B1821-24 (in M28), B1937+21. • X-ray pulsar wind nebulae of MSPs are also detected recently (PSR B1957+20, Stappers et al. 2003, Huang et al. 2007) Two origins of PWNe: • The interaction between the pulsar winds with the interstellar medium (ISM) – bow shock; • interaction between pulsar winds and the stellar winds of donor stars – intrabinary shock
MSPJ1~axX-raybehaviorof MSPsinglobularcluste1-610ObservationsshowVverysoftX-raythermalspectra,kT~0.1kev2aPreviouslythoughttohavenoX-raytailsZu2extendedto1okeV.10-的MSPO1Ao)saOnlythermalemission1_610siunoRecentChandradeepobservationsu(Bogdanovetal.2006...):Non-thermalemissionsinsomeMsPsarealsodetected!62V10MSPWOrigin:1Aay10PwNeduetotheintrabinaryshock1~610unosGas densityof isM inglobularclustersisverylow.SoPwNeonlyareobviousinbinary2systems.Most are stillthermal dominated.0.525Phaton energy (kev)
X-ray behavior of MSPs in globular clusters (e.g. Tuc 47 ) Slope =1 Slope =0.2 Observations show very soft X-ray thermal spectra, kT ~ 0.1 keV Previously thought to have no X-ray tails extended to 10 keV. Only thermal emission Recent Chandra deep observations (Bogdanov et al. 2006 .): Non-thermal emissions in some MSPs are also detected ! Origin: PWNe due to the intrabinary shock Gas density of ISM in globular clusters is very low. So PWNe only are obvious in binary systems. Most are still thermal dominated