PoS(FRAPWS2016)036 http://pos.sissa.it/ 1 [email protected] of this test conclusions sources associated with gamma-ray remnants. TeV synchrotron sources and are drawn about the evolution and lifetime of shell-type X-ray Galactic cosmic rays are generally assumed to be accelerated in supernovae and their remnants. The acceleration of the particles is attributed to their repeatedly interaction with the shock front. Model calculations have shown that a significant fraction of the supernova explosion energy can be converted to energy of cosmic rays. The feedback of this large energy transfer on the dynamical evolution and its impact on the age estimates of supernova remnants is addressed. True ages might be significantly lower than the standard Sedov ages. The impact is described Jr). byIndependent a quantitative model, which is tested on RX J0852.0-4622 (Vela Copyright owned by the author(s) under the terms of the Creative Commons Creative of by author(s)Copyright the terms the the under owned

Speaker Mondello (Palermo), Italy Mondello 1  4.0). 4.0 International (CC BY-NC-ND License Attribution-NonCommercial-NoDerivatives Frontier Research in Astrophysics – II Astrophysics in Research Frontier May23-28 2016 PR Vaterstetten Germany 8, Vaterstetten, Mozartstrasse E-mail: Supernova Remnants on their Evolution Case– onSupernova the their Remnants Jr) RX (Vela of J0852.0-4622 Aschenbach Bernd Consequences of Cosmic Ray Acceleration in Acceleration of Cosmic Consequences Ray PoS(FRAPWS2016)036 Bernd Aschenbach Bernd eV for protons. The protons. for eV

15 10 2 The three SNRs which show X-ray synchrotron emission and TeV gamma-rays are There are about 294 catalogued galactic SNRs identified as such by their radio emission, Galactic cosmic rays have been suggested to be generated in supernova remnant shock derived using the following seven relations. seven thefollowingusing derived I think, which has not been considered is so thatfar, the fairly large transfer of toenergy cosmic theSNR.thedynamicalof evolution on effect anrays should have As far as I know there is no analytic expression available to describe the cosmictime raydependence of shock acceleration. Nevertheless, there may be a reliable approximation which is front of shell-type SNRs. Among the results of the application ofSN1006 (Ksenofontov thiset al., 2005) theoryare thatfirstly, thewith energy in cosmicrespect rays can reachto 55% of the total SN the secondly, explosion accelerationenergy, time scale can range between just 300 and 700 years, depending weakly onand, the thirdly ambientthe increase energy matter density, in cosmic rays saturates after 2000 – 3000 years, and isthe notenergy replenished. In particular, concerning cosmic ray acceleration in shock fronts? shockin accelerationraycosmic concerning rays shock by of cosmic SNR acceleration 2. Creation atthe instance, for shockwithinteraction particlestheir waves´, of acceleration by diffusion-like The generation of cosmic rays in shocks is treated using the ´theory of non-linear SN1006 with both thermal and synchrotron X-ray emission and possibly TeV gamma-rays, TeV emission possibly X-rayand synchrotronthermal with both SN1006 and RX 1713.7-3946 with synchrotron X-rays, lacking thermal X-rays from the outer shock completely, and front gamma-rays,TeV and RX 0852.0-4622, again without any sign of thermal X- rays but synchrotron X-rays and TeV gamma-rays. What is special about these three SNRs Three questions arise: questions Three 1. why are there so very few objects, if cosmic ray acceleration in SNR shock fronts would be galactic source ofrays;cosmic the main foracceleration; shock required SN type of special is 2. a cloudof theexplosion aroundimportance. is 3. the environment about half of them have been detected in X-rays, much less in the optical band. But so far only three SNRs have been found to radiate synchroton X-rays and gamma-raysTeV from regions confined to their shock fronts. There are synchrotron X-rays, otherlike the ,sources but the emission withis from all acrossTeV the source gamma-rayextent emission and and not confined to the shock front. Therefore these sources are not considered in this study. synchrotron radiation, i.e., >1 – 2 keV, inverseand/or Compton effect ofof high energyTeV electrons gamma-rayswith background photon producedradiation, and/or the by either high energy the protons accelerated via their SNR shockgamma-rays interaction by producing TeV protons. ambientwithnuclei,predominantlycollisions nuclear 1. Introduction to up electrons for and TeV 100 to shouldreach up energies The fronts. observation channels to pin-point an individual source are the observation of hard X-ray Cosmic Ray Accelelation in SNRs – RX J0852.0-4622 (Vela Jr) Accelelation in SNRs J0852.0-4622 – RX (Vela Ray Cosmic PoS(FRAPWS2016)036 . On which 1/2.

t cr t

) (8) 3 (5) (4) (2) ( is the energy s Bernd Aschenbach Bernd

cr 2/5 (7) cr is the kinetic energy, respectively, t ] ] ) kin cr 1/5 – E – + E +

) ) dt (6) dt ) SN /n) kin 1/2 SN (1) SN

(t s ~ E ~ dt dt + E Δ 2 2 s – E – s s th 3 ~ v ~ cr cr ~ v ~ ~ v ~ ~ v ~ v + E + cr s ~ [1 – [1exp(-t/t ~ . It is an exponential with some e-fold time cr,g

kin v ~ -(E~ SN SN cr . Equation 7 shows the resulting relation between total = E /E + E + 1/2 cr SN th t , s v , is the increase of the velocity of an ambient proton by crossing cr cr,g v v is the thermal energy and E Δ th . s v Δ E dE dE . Subsequent crossings of the particle can increase its velocity, but of varying amount, E cr,g v explosion cloud, i.e., the shock front, slows down with time t, indicated by the shock radiust.to less than proportional increasing r const r = (E 3. Modification of the Sedov relation The general view of the dynamical evolution of SNRs is that the expansion of the explosion of a SN propagating into the ambient environment starts with a phase of free expansion, which at some time, depending on the ambient matter density changes ton, the so-called Sedov-phase, which is energy conservation dominated and during which the expansion velocity of the depends on the up-stream magnetic field, its and morphology, the up-stream matter density, the injection rate of suprathermal particles and their velocity distribution. Comparison with the results of the non-linear theory done for SN1006 by Ksenofontonov et al. (2005) shows an bad is too approximation. notcontent growthanray energy cosmic that exponential of fact, it is a diffusion-like process in velocity space. Diffusion-like processes vary with incremental scale, the result is Eq 2. Eq. 3 isenergy space,obtained by bysquaring changing from velocity space to cosmic ray energy and SN explosion E process of accelerating ambient particles extracting velocity and energy from the shock and the associated magnetic field for a single crossing, though. Equation 2 is an attempt to describe the process progression, i.e., how the velocity of the suspected cosmic ray particle grows with time, Δ even slowing down its velocity, Thisoccasionally. is why the process is non-linear in time. In The shock velocity is the shock which eventually becomes a cosmic ray particle,reservoir oft the isshock, E the time, E transferred to the ambient matter that passed the shock. Equation 1 illustrates the fundamental E Δ Cosmic Ray Accelelation in SNRs – RX J0852.0-4622 (Vela Jr) Accelelation in SNRs J0852.0-4622 – RX (Vela Ray Cosmic PoS(FRAPWS2016)036 = Sedov t century, th (10) Bernd Aschenbach Bernd changes compared to s v 1/5 )]) cr (9) )] cr the time derivative of r shows a single A [1 – [1exp(-t/t A s v (1- /t = k for each value A.of This means that the 4 2/5 = A [1 – [1exp(-t/t A = t SN Sedov 1/5 /n) (t)/E SN cr t ) = t s v using equation 10 with s v Ti signal has not been confirmed by later measurements, the analyses of 44 .This relationship takes care of the energy transfer to kinetic and thermal energy from s . The ratio of r/ v Ti Ti was found (Iyudin et al., 1998), which, because of its short life-time of 90 years led to the he immediate effect is that the age of the SNR derived from r and Sedov 4. A test object A 4. radiocarbon; the bright , the Zimbabwe star, probably observed from the Great Zimbabwe 2015). monumentFrom (Wade, Japan, there is a report that on September 12, 1271 an object as bright theas full suddenly appeared on the sky about 10 degrees above the horizon, which marks the beginning of the rise Allof Nichirenthese Buddhism.findings are consistent with the 1271.in SN a of occurrence which, however, are restricted to a point-like source. point-like are restricted to a which, however, Several findings indicate that very unusual celestial events had happened in the 13 which bemight attributedare, These amongto a nearby nitrate others, SN. precipitation markers in Arctic drilled ice cores (Burgess & Zuber, 2000); sudden increase in atmospheric (Aschenbach, 1998).A gamma-ray line excess above the background signal due to radioactive 44 conjecture that this SNR would be young, about 700 should beyears,maybe close-by, as close as and200 pc (Aschenbach et becauseal., 1999). The result ofof Iyudin et its X-ray extent al. concerning the introduction, RX 0852.0-3946 (Vela Jr) . Jr) . 0852.0-3946 introduction, (Vela RX RX 0852.0-3946 (Vela Jr) was discovered during the All-Sky-SurveyROSAT in X-rays age of the SNR could be lower than the Sedov age by reductionthis in factorage k.is Fornegligible, butlow for valueshigher ofvalues A ofthe A the age The usek=4.2.A=0.95, of thereduction Sedov A=0.90, k=2.22; A=0.7, k=1.35; = is 0.5, k=1.16; A example, significant. For age as an age estimate becomes fairly unreliable, if A is approaching values of 0.7 and more. Assuming that this is physically possible, a test object would be, as mentioned in the T t maximum for the parameter 2r/(5 E thefollowingto 10. relation the original equationthat is Sedov modified such const (E r = 2/5 r/ the shock, which causes the slow-down, but not of the energy losses pumped inAs cosmic rays. a working hypothesis I suggest that the original Sedov relation should be modified to take care willthefollowing useI relation consumption. energy raythe cosmicof Cosmic Ray Accelelation in SNRs – RX J0852.0-4622 (Vela Jr) Accelelation in SNRs J0852.0-4622 – RX (Vela Ray Cosmic Measuring the shock velocity and the shock radius the age of the SNR is estimated by PoS(FRAPWS2016)036 erg, 51 =10 , if theTeV =300 years. cr SN t E (Ksenofontov (Ksenofontov et Bernd Aschenbach Bernd and 3/16 -3 -3 for values of A >0.9. s (Katsuda et al., 2008); cm v is the distance measured . This suggests that the 1 -3 cm which could be up to 700 to 800 cr, cr, t /n (Aharonian et al. 2007) emission. d 2 the particle/cosmic ray acceleration 1 -3 = 0.84 arcsec/yr s =732 km/s . km/s . =732 cm v s decay .

; v -3 0 erg ∙ d π 5 50 r = 1° ergs, the const in equation 10 is 14 pc.Applying the 51 = 2.5∙10 cr 10 E in SN E and -3 cm (Slane et al., 2001); and the distance to the SNR is d=386 pc. The cosmic ray e-fold growth time -3 -1/2 1 cm d =338The years. values of n and d are fairly insensitive to =1536 km/s . .=1536 km/s s cr important is evident from equation 1. The relevancecomparing the loss of shockof energy to kinetic and thermal energy of the ambientshocked plasma, which density n, is obvious from increases with productionwhereas n, increases withthe cosmic n ray energy al., 2005). For a value, thanplasma transfer heating. times higher energy inwould 10 be efficiency for instance, of n=0.06 possible source or SN type Ia events. This argument expansionis speed,strengthened byexceeding the theearly generallyvery high accepted valuesshowed a mean ofexpansion velocity of 10000-2000040000 km/s averaged overkm/s. the first six SN1987A years. It appears, that a low ambient matter density and a highfavorenergy, theexplosion efficient shock velocity,acceleration ofrather particles. Thatthan the initialhigh explosion velocityexplosion is The three mentioned,SNRs i.e., RX 0852.0-4622, 1713.7-3946RX SN1006,and appear to have in common a very low ambientprogenitor star was densitynot likely to be ofa red supergiant because of something the much higher density <0.05 of the wind embedding such a star at the time of its explosion. This leaves blue supergiants as a Katsuda et al. (2008) indicate. Raising the value A toofA=0.946 the age of the remnant could The distancebe would still be 730 d=368 years. pc, the n=0.036density bethecurrent, casetoday´s, velocity would this In 5. Conclusions v Equation 10 implies that t becomes fairly insensitive to the ratio of r/ Allen et al. (2015) have measured the shock velocity and radius atrim a different position of the SNR obtaining an estimated Sedov age 1.7 times larger than the result of the measurements of n=0.041 t without changing yearsthe A for results valueslarger ofof nReconstructing and d significantly. the velocity time profile shows that the early velocity of the SNR must have been fairly high, i.e. 40000 km/s at t=20yrs and 20000 km/s at t=40 yrs. The current, today´s, velocity would be The Sedov age determined from the X-ray observation is 1714 years. If the true age would of For in units A=0.9075 t measured is required. a 1271)(SNinvalue minimumof 730 beyears 10000 years, n in modified Sedov relation (Eq. 10) it turns out that for a canonical value of n<0.029 gamma-ray emission is exclusively attributed to density andistheparticle in cmof kpc n in units 1 Cosmic Ray Accelelation in SNRs – RX J0852.0-4622 (Vela Jr) Accelelation in SNRs J0852.0-4622 – RX (Vela Ray Cosmic The measured properties of Vela Jr are PoS(FRAPWS2016)036 , 142. 396 , the lifetime is , 141. Bernd Aschenbach Bernd μG 396 . After After a couple of a . μG , Nature , Nature Ti associated with a previously a previously with associated Ti , 997. 44 H.E.S.S. Observations of the Observations H.E.S.S. 350

, A&A A&A , , 973. , 12. Dependence of the gamma-ray emission from from Dependence of emission gamma-ray the Emission from from Emission 236. Constraints of age, distance and progenitor of the of age, and progenitor distance Constraints 443 798 , L35. , L35. On the Expansion Rate, Age, and DistanceAge, of the Rate, Expansion the On 6 RX J0852.0-4622: Another Nonthermal Shell-Type NonthermalAnother Shell-Type RX J0852.0-4622: 661, 814. 278 , ApJ ApJ , , A&A A&A , 548, The Slow Rim of X-Ray the of Northwestern Expansion the ApJ ApJ , ApJ ApJ , the lifetime of the electrons producing 1 keV X-rays is http://upetd.uo.ac.za/thesis A.R. Bazer-Bachi, et al., 2007, al., et A.R. Bazer-Bachi,

, ApJ ApJ , μG Footprints of the newly discovered Vela supernova in Antarctic ice ice Antarctic in supernova Vela of discovered newly the Footprints , 1. suggested by the non-linear theory of shock acceleration, and 14 cr t Discovery remnant nearby of a young supernova Southern African Cosmogenics and Geomythology of the Great Zimbabwe and Geomythology Great the African Cosmogenics of Southern A.G. Akhperjanian, A.G.

Astroparticle Physics Supernova Remnant G266.2-1.2 (Vela Jr.) Supernova G266.2-1.2 Remnant (Vela Supernova (G266.2-1.2) Remnant Extended a Widely and Spectrum of Morphology Supernova RX J0852.0-4622: Shell-Type Remnant Source, Gamma-Ray High Energy Very Cultural Complex since the Mediaeval Trade Network Era. sinceCultural Complex Mediaeval the Trade of Pretoria, Thesis.PhD University Supernova RX J0852.0-4622 Remnant supernova remnant RX J0852.0-4622/GRO J0852-4642 remnant supernova cores? SN 1006 on the astronomical parameters 1006 on theSN astronomical supernova of a young supernovaunknown Galactic covery remnant nearby F. Aharonian, F. et DeLaney 2015, al. T. K.Allen, Chow, G. E. S. Katsuda, H. Tsunemi, K. Mori 2008, Mori K. Tsunemi, S. Katsuda, H. et 2001, al., Hughes, R.J. Edgar, J.P. Slane, P. B. Aschenbach, A. Iyudin, V. Schönfelder 1999, Schönfelder V. Iyudin, A. Aschenbach, B. 2000, &K. Zuber, Burgess C.P. 2015, Wade, R.P. B. Aschenbach 1998, B. al., et K.Bennett, 1998, V.Schönfelder, Iyudin, A.F. L.T. Ksenofontov, E.G. 2005, Berezhko, H.J.Völk Ksenofontov, L.T. [9] [7] [8] [4] [5] [6] [2] [3] [1] [10] among population. among the SNR References effect. What is left after at most brightnessa radio supernova remnant, coupleand possibly a lotof of cosmic ray aprotons, and who knows, few thousand years supernova remnant. by a apparently unaccompanied isolated is a fairly low surface The combination of low ambient density, high SNRbirth connectedshock-velocity cosmicand rayshort electrons lifetimemight of explain the rareness of this special type of SNRs 5800 years, and for those producing 10 keV X-rays the lifetime is 1800 years. If the ambient up-stream magnetic field is significantly higher than the typical galactic 5 for instance, by a of factor about fifteen for a strength field 30shorter, of few hundred years the high energy electrons energy are gone and with them the high energy X- ray synchrotron radiation and the TeV gamma-rays if associated with the inverse Compton independently in this study, the cosmicindependently rayin accelerationthis starts study, to saturate after 2000 - 3000 years without any further energy supplied because the shock velocity has become too low (c.f. Eq.1). With no further energy supply and no re-acceleration the cosmicin their electrons If they forbeing energy fairly losses radiate short. with the time-scale radiation ray particles are subject to an up-stream magnetic field of 5 Cosmic Ray Accelelation in SNRs – RX J0852.0-4622 (Vela Jr) Accelelation in SNRs J0852.0-4622 – RX (Vela Ray Cosmic Given the values of PoS(FRAPWS2016)036 Bernd Aschenbach Bernd 7 I like to forthank theRichard Wade information about the Zimbabwe event and bringing to my mind the Nichiren event, as well as Franco Giovannelli for further details of the Nichiren event. data. theradiocarbon thanksRichard who communicated mytoFirestone also I express Cosmic Ray Accelelation in SNRs – RX J0852.0-4622 (Vela Jr) Accelelation in SNRs J0852.0-4622 – RX (Vela Ray Cosmic Acknowledgement