shock cloud interaction in the vela snr the xmm newton view
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Shock-cloud interaction in the Vela SNR: the XMM-Newton view. M. Miceli 1 , F. Bocchino 2 , A. Maggio 2 , F. Reale 1 1.Dipartimento di Scienze Fisiche ed Astronomiche, Universit à di Palermo 2. INAF-Osservatorio Astronomico G. S. Vaiana di Palermo. Low spatial resolution (> 5’).

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shock cloud interaction in the vela snr the xmm newton view

Shock-cloud interaction in the Vela SNR: the XMM-Newton view

M. Miceli1, F. Bocchino2, A. Maggio2, F. Reale1

1.Dipartimento di Scienze Fisiche ed Astronomiche, Università di Palermo

2. INAF-Osservatorio Astronomico G. S. Vaiana di Palermo

interaction between the blast wave shock of a middle aged snr and the inhomogeneities of the ism
Low spatial resolution

(> 5’).

Low Aeff.

Low spectral resolution (E/DE < 2)

Low Aeff.

Geometry of the system?

No detailed comparison between X-ray and optical emission.

Difficulty in estimating the physical parameters of the plasma.

Detecting NEI effects.

Interaction between the blast-wave shock of a middle-aged SNR and the inhomogeneities of the ISM.

The analysis of past X-ray observations left many open issues:

Impossibility of unambiguously describing the physics of the shock-cloud interaction.

the data
Thedata
  • Guaranteed Time Observation.
  • Coordinates: a (2000)=8h35m44s; d (2000) = -42º35’29’’.
  • Exposure time: 26.8 ksec (PN); 31.1 ksec (MOS).
  • Mode: Extended Full Frame (PN); Large Window (MOS).
  • Filter: Medium.
slide4
Our aims:
  • Describing the morphology of the ISM clouds (shape, dimension, spatial distribution…).
  • Obtaining information about the physical properties and the internal structure of the clouds.
  • Studying the dynamics and the evolution of the shock-cloud interaction.

ROSAT All Sky Survey (0.2-2.4 keV)

slide5
EPIC count rate images

RegNE

~ 2.4 pc

0

cnt/s

7.210-5

0

cnt/s

10-4

FilD

slide6
Comparison between X-ray and optical emission in the FilD region
  • Color coding:
  • Green: Ha emission
  • Violet: OIII emission
  • Red: X-ray contour levels (0.3-0.5 keV)

Maximum X-ray contour levels are just outside the optical filament: the optical emission follows a path that grazes, without crossing, the brightest X-ray FilD regions.

slide7
Regions selected for spectral analysis

0.3-2 keV

  • Color coding:
  • Black: FilD
  • Red: South-Western region
  • Blue: RegNE

In each region the mean photon energy E has low fluctuations:

DE/Eavg  0.04

slide8
Spectral analysis

Representative folded spectrum

O/O= 1.0 ± 0.1

Ne/Ne = 1.7 ± 0.2

Fe/Fe = 0.39 ± 0.05

All spectra are well described by two MEKAL components

slide9
TII (106 K)

TI (106 K)

cnt/s

The values of the temperature of both components don’t show significant variations in the field of view.

slide10
nII2LII (1017 cm-5)

nI2LI (1017 cm-5)

cnt/s

For both components the product n2L (where n is the particle density and

L is the extension along the line of sight) presents huge inhomogeneities

in the field of view.

slide12
Evolution of the shocked clouds

n = 0.5  1.9 cm-3

T  3.0  106 K

Corona:

trad> tcond

Evaporation

Collapse

n = 3.2  8.2 cm-3

T = 3  10  104 K

Optical filament:

n = 1.4  5 cm-3

T  1.14  106 K

Core:

trad< tcond

n < 0.07 cm-3

Intercloud medium:

T = 4  8  106 K

trad> tcond

conclusions
cores: radiative cooling collapse

coronae: thermal conduction evaporation

Conclusions:
  • We resolved different phases in ISM clouds.
  • 3-D map of the observed clouds

(FilD mass  1031g for a core particle density of 2 cm-3).

  • Discriminate model (no reflected shocks).
  • Evolution of the

shocked clouds

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