SUPERNOVA REMNANTS
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SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS. JOHN R. DICKEL UNIVERSITY OF NEW MEXICO AND ROSA MURPHY WILLIAMS COLUMBUS STATE UNIVERSITY. Preliminary SNR tables at: http://hoth.ccssc.org/mcsnr/test.php. SNR IDENTIFICATION.

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SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS

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Supernova remnants in the magellanic clouds

SUPERNOVA REMNANTS

IN THE MAGELLANIC CLOUDS

JOHN R. DICKEL

UNIVERSITY OF NEW MEXICO

AND

ROSA MURPHY WILLIAMS

COLUMBUS STATE UNIVERSITY

Preliminary SNR tables at:

http://hoth.ccssc.org/mcsnr/test.php


Snr identification

SNR IDENTIFICATION

  • EXTENDED GENERALLY SHELL -LIKE OBJECT - 0.2 PC FOR 1987A TO 158 PC FOR DEM L203

    (1 PC IS 4 ARCSEC AT THE LMC AND 3.4 ARCSEC AT THE SMC)

  • NON THERMAL RADIO SPECTRA - TYPICAL SPECTRAL INDICES,  = -0.5,

    WHERE Sf = const f

  • THERMAL X-RAYS - TYPICAL TEMP ~ 1 keV WITH A LARGE SPREAD

  • CAVEAT - PULSAR WIND NEBULAE HAVE FLATTER RADIO SPECTRA AND NON-THERMAL HIGH ENERGY X-RAY TAILS

  • [S II]/ Ha > 0.4


Supernova remnants in the magellanic clouds

= -0.48

DEM L81

= 0.0


X ray spectrum of n103 snr usually incorrectly called n103b

X-RAY SPECTRUM OF N103 SNR(usually incorrectly called N103B)

THIS SHOWS THE THERMAL NATURE OF THE EMISSION

LEWIS, K. ET AL. 2003 ApJ, 582, 770


Supernova remnants in the magellanic clouds

SNR MCELS J0521-6542

3 COLOR

RATIO

[S II] H

[S II]/H


Type classification of magellanic cloud snrs

TYPE CLASSIFICATION OF MAGELLANIC CLOUD SNRS

CORE COLLAPSE:

PRESENCE OF A PULSAR OR OTHER COMPACT REMAINS

IN A REGION OF YOUNG STARS

OXYGEN RICH

TYPE Ia:

XRAY SPECTRA SHOW LINES OF HIGHLY IONIZED INTERMEDIATE MASS ELEMENTS

BALMER DOMINATED IN OPTICAL


Supernova remnants in the magellanic clouds

0540-693 - A PROTOTYPE COMPOSITE SNR

50-MSEC PULSAR, PWN, O-RICH SHELL,

ORGANIZED POLARIZATION IN THE PWN

6-CM RADIO IMAGE


N157b another composite

N157B ANOTHER COMPOSITE

Radio - contours are

2,3,4,6,7 nJy/beam

X-ray - contours are 5,10,20,30,40,100,300,600 counts from 0.1-10 keV

The shell can be seen faintly on the southern part of the radio image.

The 16-msec X-Ray pulsar is at the center of the bright X-Ray contours and at the position of the cross in the radio image.


Spectrum of n157b

SPECTRUM OF N157B

IT WILL BE VERY DIFFICULT TO MAKE ONE CONTINUOUS

SPECTRUM FOR THIS OBJECT


X ray spectrum of n103 snr note the many lines of highly ionized intermediate mass elements

X-RAY SPECTRUM OF N103 SNRNOTE THE MANY LINES OF HIGHLY IONIZED INTERMEDIATE-MASS ELEMENTS

LEWIS, K. ET AL. 2003 ApJ, 582, 770


H line profile toward the type ia balmer dominated snr 0519 675

H LINE PROFILE TOWARD THE TYPE Ia BALMER-DOMINATED SNR 0519-675

UNEQUILIBRATED VELOCITY 1180 KM/S

EQUILIBRATED 1580 KM/S

SMITH, R. C. ET AL. 1991, ApJ, 375, 652


N19 area in the smc

N19 AREA IN THE SMC

JY/BEAM

RED: X-RAY CONTOURS GREYSCALE: 13-CM RADIO


N19 area in three wavelengths

N19 AREA IN THREE WAVELENGTHS

H22cm Radio 1.5 - 8 keV X-ray


Some statistics

SOME STATISTICS

LMCSMC

TOTAL NUMBER OF SNRS4919

CORE COLLAPSE 12 4

TYPE Ia 61

UNKNOWN 3114

STANDARD STATISTICS EXPECTED IN IRREGULAR GALAXIESPREDICT ABOUT 10% TYPE Ia SNe.


Radio luminosity vs diameter for lmc snrs

RADIO LUMINOSITY vs DIAMETER FOR LMC SNRs

slope -1.13

corr coef 0.08

1987A

DEM L71

CONCLUSION: THERE IS NO CORRELATION OF

LUMINOSITY WITH DIAMETER (IN AGREEMENT WITH PREVIOUS STUDIES)


X ray radio luminosities of lmc snrs

X-RAY - RADIO LUMINOSITIES OF LMC SNRs

DEM L71

DEM L71

slope 0.77

corr. coeff 0.41

CONCLUSION: BRIGHTER X-RAY EMISSION MAY, IN GENERAL, CORRESPOND TO BRIGHTER RADIO BUT THERE IS NO CLEAR CORRELATION


1 1 kev 2kev 5 kev

CHANDRA IMAGE OF CAS A

1.1 keV 2keV 5 keV


X ray image and radio contours of the oxygen rich snr n132d the brightest lmc radio source

X-RAY IMAGE AND RADIO CONTOURS OF THE OXYGEN RICH SNR N132D, THE BRIGHTEST LMC RADIO SOURCE


Snr 1e0102 72 3 in the small magellanic cloud

SNR 1E0102-72.3 in the Small Magellanic Cloud

radioX-ray

optical in the light of [O III] characteristic of oxygen rich SNRs

Note that the radio shell lies outside the X-ray one – an unusual condition in shell SNRs.


Supernova remnants in the magellanic clouds

THE MAGELLANIC CLOUD CANDIDATES ARE ABOUT 20 TIMES FURTHER AWAY THAN CAS A SO THE REQUIRED SENSITIVITY NEEDS TO BE INCREASED BY A FACTOR OF 400.THE INTERNATIONAL X-RAY OBSERVATORY (IXO) WILL BE ABOUT 100 TIMES MORE SENSITIVE THAN CHANDRA THEREFORE WITH MODESTLY LONGER EXPOSURES THE FIRST TASK FOR IXO SHOULD BE TO FIND THE COOLING NEUTRON STARS IN N132D AND 1E0102-723.

THE REWARD FOR DOING SO: A BOTTLE OF EITHER DICKEL TENNESSEE WHISKEY OR GRUET NEW MEXICO CHAMPAGNE


Supernova remnants in the magellanic clouds

Preliminary SNR tables at:http://hoth.ccssc.org/mcsnr/test.phpPlease send us references, new data, etc.We will eventually get proper pages for each SNR.


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