Pulsar wind nebulae and their interaction with the

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Pulsar wind nebulae and their interaction with the environments Fangjun Lu 卢方军 Institute of

Pulsar wind nebulae and their interaction with the environments Fangjun Lu 卢方军 Institute of High Energy Physics Chinese Academy of Sciences

Most of the spin-down power of a pulsar is not released through direct radiation

Most of the spin-down power of a pulsar is not released through direct radiation (Li, Lu, & Li 2008, Ap. J 682, 1166)

http: //chandra. harvard. edu/ Most (90%) of the spin-down power of a pulsar is

http: //chandra. harvard. edu/ Most (90%) of the spin-down power of a pulsar is released via a relativistic wind.

The basic configuration of a PWN Pulsar • Pulsar wind Therefore, the properties of

The basic configuration of a PWN Pulsar • Pulsar wind Therefore, the properties of a pulsar Terminal shock wind nebula are highly determined Pulsar wind nebula by the composition and geometry of Interface with the pulsar wind as well Interstellar as the. Medium interaction with the environments. The magnetized pulsar wind leaves the pulsar with almost the speed of c (γ~103 -106). • A termination shock forms at the radius where the wind rampressure balances the pressure of the environments, and over there the particles are randomized ( and probably accelerated) and begin to emit synchrotron photons. • The PWN is a magnetized particle bubble surrounded by the ISM. ( Rees & Gunn 1974)

Outline • A statistical study of the X-ray emission of young pulsars and pulsar

Outline • A statistical study of the X-ray emission of young pulsars and pulsar wind nebulae. • Pulsar wind nebulae in various conditions: – “Freely” expands; – Within a supernova remnant; – Moves supersonically in space; – In highly organized magnetic field; – In high velocity interstellar wind.

A statistical study with a sample of 27 pulsars Li, Lu & Li 2008,

A statistical study with a sample of 27 pulsars Li, Lu & Li 2008, Ap. J 682, 1166

A statistical study with a sample of 24 PWNe Li, Lu & Li 2008,

A statistical study with a sample of 24 PWNe Li, Lu & Li 2008, Ap. J 682, 1166

Relations between the X-ray luminosity and spin-down power The more energetic pulsars intend to

Relations between the X-ray luminosity and spin-down power The more energetic pulsars intend to release a bigger fraction of their spin-down power in their PWNe. Li, Lu & Li 2008, Ap. J 682, 1166

Relations between the X-ray luminosity and the photon index Apparently, there is a negative

Relations between the X-ray luminosity and the photon index Apparently, there is a negative correlation between the Xray luminosity and spectral index for pulsars, while a positive correlation holds for the PWNe. Li, Lu & Li 2008, Ap. J 682, 1166

Pulsare PWNe Younger (more energetic) pulsars tend to have harder spectra from their magnetosphere,

Pulsare PWNe Younger (more energetic) pulsars tend to have harder spectra from their magnetosphere, while softer spectra from their wind nebulae Li, Lu & Li 2008, Ap. J 682, 1166

What do these results tell us about the physics of pulsars and PWNe, besides

What do these results tell us about the physics of pulsars and PWNe, besides these empirical formulae?

Physical implications • The photon indices between 2 and 3 for pulsars pose question

Physical implications • The photon indices between 2 and 3 for pulsars pose question on all the current pulsar models. Because the cascade never produces X-ray emission with photon index higher than 2. • The spectral index of synchrotron photons is between (p+1)/2 to (p+2)/2 from the slow-cooling regime to the fast-cooling regime. The photon indices of the PWNe strongly favor an electron index of p~2. 2, well consistent with theoretical predictions on particle acceleration in relativistic collisionless shocks. So the termination shock does accelerate electrons. The γfactor of the wind is probably much smaller than 106. • The PWNe of the more energetic pulsars tend to have higher magnetic field in the nebulae, which gives higher synchrotron efficiency and softer X-ray spectrum of the nebula. But it is not the case for the X-ray emission of the pulsars.

PWNe in various environment conditions

PWNe in various environment conditions

Interfaces The morphology of a PWN is determined by the geometry of the pulsar

Interfaces The morphology of a PWN is determined by the geometry of the pulsar wind and the distribution of the ISM surrounding the PWN. or The X-ray image represents the distribution of fresh wind particles, and the X-ray spectral evolution traces the particle flow. The radio images could be affected by the distribution of the aged particles.

SNR G 54. 1+0. 3: A PWN without significant confinement Pulsar G 54. 1+0.

SNR G 54. 1+0. 3: A PWN without significant confinement Pulsar G 54. 1+0. 3 is powered by the 136 ms pulsar in the center. The Chandra X-ray image shows bright ring surrounding the pulsar, and two elongations roughly perpendicular to the ring. The wind of the central pulsar can be divided into two components: equatorial flow and polar flow. (Lu et al. 2002)

The downstream velocity could be derived as 0. 4 c by fitting the brightness

The downstream velocity could be derived as 0. 4 c by fitting the brightness variations, which means that the wind is particle dominated. (Lu et al. 2002)

(Lang, Wang, Lu, & Clubb 2010) The X-ray and radio images look very much

(Lang, Wang, Lu, & Clubb 2010) The X-ray and radio images look very much similar to each other, and the magnetic field is well organized.

The radio and X-ray extents are almost the same for G 54. 1+0. 3.

The radio and X-ray extents are almost the same for G 54. 1+0. 3. (Lang, Clubb, Lu, & Wang 2009)

 • Similarity of the radio and X-ray morphology: there is no significant accumulation

• Similarity of the radio and X-ray morphology: there is no significant accumulation of old particles. • Similar radio and X-ray sizes: the size of the nebula is determined mainly by the diffusing of the particles rather than by their lifetime. The quick diffusion lowers both the particle number density and the magnetic field (if we assume equipartition) and so the radio synchrotron brightness decreases very rapidly. G 54. 1+0. 3 is very weakly confined by the environment

PSR B 1951+32 The PWN of PSR B 1951+32 is in the center of

PSR B 1951+32 The PWN of PSR B 1951+32 is in the center of SNR CTB 80.

S II O III (Hester & Kulkarni 1989) Hα Log (OIII/H α) & H

S II O III (Hester & Kulkarni 1989) Hα Log (OIII/H α) & H α In the center of CTB 80 (surrounding the pulsar), small nebulae have been detected in optical emission lines.

Radio image of core of CTB 80 Chandra X-ray image Migliazzo et al. (2002)

Radio image of core of CTB 80 Chandra X-ray image Migliazzo et al. (2002) Li, Lu & Li (2005) The PWN of PSR B 1951+32 shows a shell-like structure in both radio and Xrays, suggesting strong confinement by the SNR ejecta. The high brightness region is well within the OIII and S II line filaments, while the Hα filaments define the edge of the low brightness region.

X-ray tail Termination shock Shell Pulsar Contours: X-ray Greyscale: Radio The PWN is produced

X-ray tail Termination shock Shell Pulsar Contours: X-ray Greyscale: Radio The PWN is produced by the supersonically moving pulsar in SNR ejecta. (Li, Lu, & Li 2005)

We find intriguing spectral hardening in regions of the radio and X-ray shell, which

We find intriguing spectral hardening in regions of the radio and X-ray shell, which can only be explained by the new particle acceleration. This shows that the pulsar wind bubble can expand supersonically and generate shocks, even in such an old (5× 105 yr) system. The optical filaments are also produced by the shock wave propagating into the ejecta and the interstellar medium. (Li, Lu, & Li 2005)

G 359. 94 -0. 04: A cometary PWN near the Galactic Center Chandra X-ray

G 359. 94 -0. 04: A cometary PWN near the Galactic Center Chandra X-ray image of the Galactic center. X-ray contours overlaid on the IR image (Wang, Lu, & Gotthelf 2006)

(van der Swaluw et al. 2003) (Gaensler et al. 2004) When a pulsar moves

(van der Swaluw et al. 2003) (Gaensler et al. 2004) When a pulsar moves supersonically in the ISM, a bow shock will be running into the ISM, a termination shock will be ahead of the pulsar, and most of the pulsar wind will be confined to the direction opposite to the pulsar proper motion. The radius of the termination shock is determined by the spin-down power and proper motion velocity of the pulsar as well as the ISM density.

Linear brightness profile Photon index evolution The cometary morphology is a sign of the

Linear brightness profile Photon index evolution The cometary morphology is a sign of the ram-pressure confined PWN. The spectral steepening with increasing distance from the point source further confirms such an identification.

HESS Te. V Observation of the Galactic Center Region G 359. 95 -0. 04

HESS Te. V Observation of the Galactic Center Region G 359. 95 -0. 04 HESS J 1745 -290

Evidence for G 359. 95 -0. 04 (rather than Sgr A*) as the counterpart

Evidence for G 359. 95 -0. 04 (rather than Sgr A*) as the counterpart of HESS J 1745 -290 • Many PWNe are observed as Te. V sources. • G 359. 95 -0. 04 is consistent with HESS J 1745 -290 positionally. • G 359. 95 -0. 04 can contribute comparable Te. V flux through inverse compton scattering to the ambient seed photons (Wang et al. 2006, Hinton & Aharonian 2007, Ap. J 657, 302). • HESS J 1845 -290 does not show any variation, especially when Sgr A* (the other candidate) experiences flares (Hinton et al. 2007, @ICRC 30).

Radio map of the GC region • Non-thermal filaments almost perpendicular to the Galactic

Radio map of the GC region • Non-thermal filaments almost perpendicular to the Galactic Plane. • The origin of the high energy particles has been a long time mystery.

X-ray G 0. 13 -0. 11: A pulsar wind nebula in strong organized magnetic

X-ray G 0. 13 -0. 11: A pulsar wind nebula in strong organized magnetic field Wang, Lu & Lang 2002

G 0. 13 -0. 11 leads a bunch of NTFs (the GC arc)

G 0. 13 -0. 11 leads a bunch of NTFs (the GC arc)

Spectral index variation of the GC arc.

Spectral index variation of the GC arc.

Spectral index variation of the GC arc Reflects the aging of the high energy

Spectral index variation of the GC arc Reflects the aging of the high energy particles with increase distance from the pulsar. G 0. 13 -0. 11 is probably a PWN in strong organized magnetic field.

The X-ray emission of G 359. 54+0. 18 Lu, Wang & Lang 2003 Pulsar

The X-ray emission of G 359. 54+0. 18 Lu, Wang & Lang 2003 Pulsar wind particles could also illuminate the non-thermal radio filaments in the Galactic Center region.

A deep Chandra image of the GC region.

A deep Chandra image of the GC region.

Morphological properties (Lu, Yuan, & Lou 2008)

Morphological properties (Lu, Yuan, & Lou 2008)

Their spectra are nonthermal. F 1 -F 10 (Lu, Yuan, & Lou 2008)

Their spectra are nonthermal. F 1 -F 10 (Lu, Yuan, & Lou 2008)

Main morphological and spectral properties of the filaments • Most of the filaments contain

Main morphological and spectral properties of the filaments • Most of the filaments contain point-like sources at their heads. • All. The the filaments cometaryare morphology. X-ray show filaments most • The spectra are non-thermal, with photon indices probably close to Sgr A* and 1. 0 -2. 5, Lx 1032 to 1034 erg/s, and absorption powered by 23 pulsars younger column density 10 cm-2. 5 yrs. counts, a spectral softening • When there are enough than 3*10 with distance from the point-like source can be detected.

Star formation rate 15 pulsars younger than 3*105 yrs within 7 pc from Sgr

Star formation rate 15 pulsars younger than 3*105 yrs within 7 pc from Sgr A* => Star formation rate of 6*10 -4 solar mass yr-1, ~100 times higher than the mean star formation rate of the Galaxy.

There. Arches are many massive stars in the GC region. The cluster Quintuplet cluster

There. Arches are many massive stars in the GC region. The cluster Quintuplet cluster mass function of stars in this region suggests a star formation rate of 10 -7 solar mass yr-1 pc-3, about 250 times higher than the mean of the Galaxy, consistent with our estimate basing on the number of X-ray PWNe in this region.

Galactic Plane Sgr A* Most of the X-ray filament tails point away from Sgr

Galactic Plane Sgr A* Most of the X-ray filament tails point away from Sgr A*

 • The fact that most of the X-ray filament tails point away from

• The fact that most of the X-ray filament tails point away from Sgr A* suggests that there exists a radial flow from GC. This flow (Galactic wind) blows the pulsar wind particles to the anti-GC direction and shapes the cometary morphology. These filaments thus represent PWNe in strong windy environment. • Since the pulsars are expected to move in random directions with peculiar velocities of ~400 km/s, the speed of the Galactic wind should be comparable to or greater than ~400 km/s.

Summary • The luminosity of the PWN is positively correlated with the spindown power

Summary • The luminosity of the PWN is positively correlated with the spindown power of the pulsar. So PWNe are usually detected for young pulsars. • The morphology of a PWN is determined by the interaction with the environment. If the pulsar – is in a low density cavity, then the structure of the PWN reflects mainly the pulsar wind geometry. – is surrounded by the SNR ejecta, the wind materials will be well confined, and the expansion of the PWN can generate a strong shock into the ejecta. – moves supersonically in the ISM, the PWN will be like a comet with the tail points to the opposite direction of the pulsar proper motion. – locates in strong organized magnetic field, the PWN may well trace the structure of the magnetic field. • The filamentary PWNe in the Galactic center shows that the star formation rate of the Galactic Center region is about 100 times higher than the mean of the Galaxy. It is also shown that there is a high velocity radial Galactic wind.