A new image from NASA's Chandra X-ray Observatory shows a supernova
remnant with a different look. This object, known as SNR 0104-72.3
(SNR 0104 for short), is in the Small Magellanic Cloud, a small
neighboring galaxy to the Milky Way. Astronomers think that SNR 0104
is the remains of a so-called Type Ia supernova caused by the
thermonuclear explosion of a white dwarf.
In this composite made of X-rays from Chandra shown in purple and
infrared data from Spitzer shown in green and red, SNR 0104 looks
unlike other likely Type Ia remnants found in our own Galaxy. While
objects such as the Kepler and Tycho supernova remnants appear
circular, the shape of SNR 0104 in X-rays is not. Instead, the image
is dominated by two bright lobes of emission (seen to the upper right
and lower left). The large amount of iron in these lobes indicates
that SNR 0104 was likely formed by a Type Ia supernova.
One possible explanation for this structure is that the explosion of
the white dwarf itself was strongly asymmetrical and produced two jets
of iron. Another possibility is that the complicated environment seen
in the image is responsible. The green shells on the left and right
side of SNR 0104 correspond to surrounding material that has been
swept up by the explosion. So, the unusual shape of the remnant might
be caused by a lack of material to the north and south of the star to
interrupt the outward path of the stellar debris. This explanation,
however, is still in question and scientists hope more data from
Chandra and other telescopes will help settle the debate.
The presence of a nearby massive star and the shells of gas and dust
seen in the wide-field view from Spitzer shows that SNR 0104 might be
located within a star-forming region. This suggests that SNR 0104 may
belong to a little-studied class of so-called "prompt" Type Ia
supernovas caused by the demise of younger, more massive stars than
average. Again, more data will be needed to test this theory.
| Fast Facts for SNR 0104-72.3: |
| Credit |
X-ray (NASA/CXC/Penn State/S.Park & J.Lee); IR (NASA/JPL-Caltech) |
| Release Date |
June 09, 2009 |
| Scale |
Full field image is 32.4 arcmin across |
| Category |
Supernovas & Supernova Remnants |
| Coordinates (J2000) |
RA | Dec |
| Constellation |
Tucana |
| Observation Date |
January 27, 2008
|
| Observation Time |
15 hours 20 minutes |
| Obs. ID |
9100
|
| Instrument |
ACIS
|
| Color Code |
X-ray (Purple); IR (Green, Red) |
| Distance Estimate |
About 190,000 light years (in the SMC)
|
|
The Chandra website is a wonderful source, offering some additional information in their releases to explain each observation. Thank you very much for the exciting results.
Posted by Stan on Saturday, 08.14.10 @ 16:57pm
I want to say thank you for this.
Posted by Frorellan on Saturday, 10.10.09 @ 21:45pm
Julian Moore
Some theoretical models suggest that the white dwarf binary system can produce strong outflow material which significantly alters the ambient medium. The stellar
rotations might play a role there. This could affect the shape of the blast wave and/or the expelled ejecta. Because the IR data show complex "shells" and "filaments" nearby this SNR, and we see evidence for non-uniform ambient
medium around this SNR, stellar winds from the progenitor/companion star
or some outflows from the binary system could have affected the surroundings.
However, we have no direct information on the companion star's nature with the current X-ray data.
S. Park (the scientist leading the study)
Posted by S. Park on Thursday, 07.9.09 @ 10:22am
Plamen Fiziev
The size of the SNR in N-S elongation (which are mostly Fe ejecta) is ~85 light years, assuming the distance of ~200000 ly to the host galaxy SMC.
S. Park (the scientist leading the study)
Posted by S. Park on Thursday, 07.9.09 @ 10:21am
benjamin landa
Did you mean "this supernova remnant" (rather than "this galaxy")? Assuming that you mean "supernova remnant", yes, there are some other metal species than Fe that are abundantly produced in the SN explosion, e.g., O, Ne, Mg, Si, S etc. Since Type Ia SNe are the major factory to produce Fe material (also Si, S, but not much O and Ne), Fe is usually a iconic element in Type Ia SNRs. In this SNR 0104, Fe is actually the most prominent element detected in X-rays. In contrast, O and Ne are typically the most abundant elements produced in "core-collapse (Types II,Ib/c)" SNRs.
S. Park (the scientist leading the study)
Posted by S. Park on Thursday, 07.9.09 @ 10:19am
Norm Guarni
Our results point at a Type Ia SN for the origin of 0104.
Type Ia SNe are thought to be caused by an explosion of a white dwarf (WD), either by accretion from the normal companion or by merging it with another WD, when they are in a close binary system. In many cases, stars are in multiple system with two or more stars, thus it may be possible that 0104 originated from such a system. We can't provide a conclusive answer with the current data,
though.
S. Park (the scientist leading the study)
Posted by S. Park on Thursday, 07.9.09 @ 10:18am
Awesome.
Posted by lucy on Thursday, 06.25.09 @ 22:27pm
Thanks space tech science, thanks NASA for your powerful work.
Posted by diakite mamadou b on Friday, 06.19.09 @ 16:25pm
It is a beautiful picture.
Posted by James Brown on Tuesday, 06.16.09 @ 12:06pm
We must wait for more data about this source to complete answer this questions guys.
Posted by Donis on Tuesday, 06.16.09 @ 09:34am
Listen, you guys are the experts, so my apologies for proposing some explanation for the irregular supernova remnant, that may be completely absurd BUT is it at all possible that this could have been a multiple star system with a minimum of three stars in very close proximity to one another, close enough to have been annihilated along with the white dwarf supernova and whose gravity caused the distortion in the resulting debris.
Thanks for all the great work.
This is one governmental area where I have no problem with my tax dollars being spent.
Have a great day
Posted by Norm Guarni on Monday, 06.15.09 @ 09:26am
Are there any other heavy metal elements that may also play a role in contributing to the sgape of this galaxy?
Posted by benjamin landa on Monday, 06.15.09 @ 01:57am
Extremely interesting.
What is the size of the double jet?
Posted by Plamen Fiziev on Thursday, 06.11.09 @ 10:51am
I'm so lucky have the chance to recognize abundant messages of the universe from this exciting wonderful good website.
Posted by chiang kuo-yan on Wednesday, 06.10.09 @ 21:00pm
As usual, the picture was terrific.
Can't wait for my grandson to see it. I've been cataloging all Chandra e-mail and photos for him in the hopes that he loves Astronomy as much as I.
KEEP UP THE GREAT WORK.
BILL
Posted by bill brookings on Wednesday, 06.10.09 @ 14:43pm
Could it be a function of dwarf angular momentum fast spinners confine debris better than e. g. slow spinners tidally locked to a closer bigger more massive companion star?
Any info on the companion star accretion source?
Posted by Julian Moore on Wednesday, 06.10.09 @ 12:02pm