A<i>SUZAKU</i>X-RAY STUDY OF THE PARTICLE ACCELERATION PROCESSES IN THE RELATIVISTIC JET OF BLAZAR Mrk 421

Garson, A.; Baring, Matthew G.; Krawczynski, H.

doi:10.1088/0004-637x/722/1/358

Cited by 20 publications

(25 citation statements)

References 57 publications

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“…They analyzed the spectrum with a parametric forward-fitting synchrotron model and with a particle acceleration model and discussed the possibilities in the context of diffusive acceleration of electrons. The third observation, ID 703043010, begun on 5 May 2008, was analyzed by Garson et al (2010) and they found that a broken power-law model fit the spectra very well.…”

Section: Discussionmentioning

confidence: 99%

“…Suzaku consists of: the X-ray Imaging Spectrometer (XIS, Koyama et al 2007) for the 0.2−10 keV low energy band; the Hard X-ray Detector (HXD, Takahashi et al 2007;Kokubun et al 2007), which utilizes PIN silicon diodes and is sensitive over 12−60 keV; and the GSO scintillator, which extends the detection ability to hundreds of keV. Mrk 421 was observed three times by Suzaku on 2006 April 28 (ID 701024010), 2008 May 5 (ID 703043010) and 2008 December 3 (ID 703020010) (Ushio et al 2009(Ushio et al , 2010Garson et al 2010). The observations are listed in Table 1 in order of the ObsID and the total elapsed time.…”

Section: Suzaku Archival Data Reductionmentioning

confidence: 99%

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X-Ray Intraday Variability of the TeV Blazar Mrk 421 with Suzaku

Zhang

Gupta

Gaur

et al. 2019

ApJ

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We present X-ray flux and spectral analyses of the three pointed Suzaku observations of the TeV high synchrotron peak blazar Mrk 421 taken throughout its complete operational duration. The observation taken on 5 May 2008 is, at 364.6 kiloseconds (i.e., 101.3 hours), the longest and most evenly sampled continuous observation of this source, or any blazar, in the X-ray energy 0.8 -60 keV until now. We found large amplitude intra-day variability in all soft and hard bands in all the light curves. The discrete correction function analysis of the light curves in soft and hard bands peaks on zero lag, showing that the emission in hard and soft bands are cospatial and emitted from the same population of leptons. The hardness ratio plots imply that the source is more variable in the harder bands compared to the softer bands. The source is harder-when-brighter, following the general behavior of high synchrotron peak blazars. Power spectral densities of all three light curves are red noise dominated, with a range of power spectra slopes. If one assumes that the emission originates very close to the central super massive black hole, a crude estimate for its mass, of ∼ 4 × 10 8 M ⊙ , can be made; but if the variability is due to perturbations arising there that are advected into the jet and are thus Doppler boosted, substantially higher masses are consistent with the quickest seen variations. We briefly discuss the possible physical mechanisms most likely responsible for the observed flux and spectral variability.

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Section: Discussionmentioning

confidence: 99%

Section: Suzaku Archival Data Reductionmentioning

confidence: 99%

X-Ray Intraday Variability of the TeV Blazar Mrk 421 with Suzaku

Zhang

Gupta

Gaur

et al. 2019

ApJ

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“…These non-detections of time lags might be due to the fact that the actual time lag is likely intra-day, which is difficult to resolve using our light curves of several-day time resolution. In Garson et al (2010), two flares of Mrk 421 lasting for 0.5 days showed several-hour time lags between the 0.5-2 keV and 2-10 keV light curves, and displayed different movements in the hardness-flux plot. Krawczynski et al (2000) indicated that the time lag between 3 keV and 25 keV is smaller than 15 hours in Mrk 501.…”

Section: Electron Spectral Hysteresismentioning

confidence: 99%

Systematic Investigation of X-Ray Spectral Variability of TeV Blazars during Flares in the RXTE Era

Wang

Xue

Zhu

et al. 2018

ApJ

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Utilizing all the 16-year RXTE observations, we analyze the X-ray spectra of 32 TeV blazars, and perform a systematic investigation of X-ray spectral variability for the 5 brightest sources during their major flares that lasted several days. We obtain photon spectral index (α), flux and synchrotron radiation peak energy (E p ) from empirical spectral fitting, and electron spectral index (p) from theoretical synchrotron radiation modeling. We find that both α and p generally display a harder-when-brighter trend, confirming the results of many previous works. Furthermore, we confirm and strengthen the result that p must vary in order to explain the observed X-ray spectral variability during flares, which would have useful implications for interpreting the associated higher-energy spectral variability. We see apparent electron spectral hysteresis in many but not all p-flux plots that takes a form of "loop" or oblique "8". We obtain a tight p-hardness ratio (HR) relation and a tighter p-α relation using spectra of flaring periods, both of which are also applicable to stacked data of quiescent periods. We demonstrate that these two empirical relations can be used efficiently to estimate p from HR or α that is readily achieved. Finally, we find that, when considering TeV blazars as a whole, α and X-ray luminosity are positively correlated, E p is negatively correlated with p and α, and E p is positively correlated with HR; all these correlations are in line with the blazar sequence. However, after correcting for the Doppler boosting effect, α and intrinsic X-ray luminosity follow an anti-correlation.

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“…Fig. 6 of Garson et al (2010) displays both clockwise and tilted figure-8 hysteresis in 0.5−2 keV Suzaku data spanning several hours for modest Mrk 421 activity over 4 days in May 2008, a period when the source did not exhibit strong flares. More recently, Figs.…”

Section: Case 1: Variation Of Injection Luminositymentioning

confidence: 99%

Multi-wavelength Variability Signatures of Relativistic Shocks in Blazar Jets

Böttcher

Baring

2019

ApJ

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Mildly-relativistic shocks that are embedded in colliding magnetohydrodynamic flows are prime sites for relativistic particle acceleration and production of strongly variable, polarized multi-wavelength emission from relativistic jet sources such as blazars and gamma-ray bursts. The principal energization mechanisms at these shocks are diffusive shock acceleration and shock drift acceleration. In recent work, we had self-consistently coupled shock acceleration and radiation transfer simulations in blazar jets in a basic one-zone scenario. These one-zone models revealed that the observed spectral energy distributions (SEDs) of blazars strongly constrain the nature of the shock layer hydromagnetic turbulence. In this paper, we expand our previous work by including full time dependence and treating two zones, one being the site of acceleration, and the second being a larger emission zone. This construction is applied to multiwavelength flares of the flat spectrum radio quasar 3C 279, fitting snap-shot SEDs and generating light curves that are consistent with observed variability timescales. We also present a generic study for the typical flaring behavior of the BL Lac object Mrk 501. The model predicts correlated variability across all wavebands, but cross-band time lags depending on the type of blazar (FSRQ vs. BL Lac), as well as distinctive spectral hysteresis patterns in all wavelength bands, from mm radio waves to gamma-rays. These evolutionary signatures serve to provide diagnostics on the competition between acceleration and radiative cooling.

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ASUZAKUX-RAY STUDY OF THE PARTICLE ACCELERATION PROCESSES IN THE RELATIVISTIC JET OF BLAZAR Mrk 421

Cited by 20 publications

References 57 publications

X-Ray Intraday Variability of the TeV Blazar Mrk 421 with Suzaku

X-Ray Intraday Variability of the TeV Blazar Mrk 421 with Suzaku

Systematic Investigation of X-Ray Spectral Variability of TeV Blazars during Flares in the RXTE Era

Multi-wavelength Variability Signatures of Relativistic Shocks in Blazar Jets

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