P/2010 A2 (LINEAR)


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The dust/debris structure is still very constant, 37 arc sec  in PA 278. The image of the Hubble Space Telescope of January,29 2010
is showing the corresponding asteroids on the Eastern part of the dust. Since this image of the Hubble Space Telescope was taken it is clear,
that the dust/debris/boulder structure is directed relatively to the Sun (Sun Pos.Angle PA 292.3 at Jan, 19 2010).

This means, that the dust/debris of P/2010 A2 (LINEAR) is not comparable with a "normal" dust tail of a comet, which is normally directed
roughly vice versa to the Sun Pos. Angle. The ejected material of the collision should be more compact than comet material.
But it seems, that the dust/debris of P/2010 A2 is influenced by both the solar wind and gravitational forces anyway.

At the moment of the assumed collision of two asteroids, the direction of the dust/debris is influenced by the impact event, off course.
But it is very interesting, that the remaining dust/debris complex is still very constant in shape and orientation.

Hiroki Akisawa from Japan calculated by Bessel-Bredikhin theory and fitted for this image.
Description of his diagram: Yahoo Comets ML      

P/2010 A2 (LINEAR) � by Bernhard Haeusler, Germany

(C) 2010-03-11 by Bernhard Haeusler, Maidbronn, Germany                                              image frozen on stars and dust structure

20 x 3 min. exposure, 2010-03-11 UT 20:32, 12" SCT  f-5.65 + CCD ST10XME
head of the dust structure on the left: 19.3 mag, "tail": 37" in PA 278�
The Sun Pos.Angle at the time of the exposure was PA 275.7 (See: HORIZON Query,
QUANTITIES=1,9,16)

P/2010 A2 (LINEAR) � by Bernhard Haeusler, Germany

Gif animation  20 x 3 minutes in reality, foreshortend to 1.8 seconds
P/2010 A2 in the center left, asteroid 19610 Arthurdent (17.4 mag) on the right upper corner

P/2010 A2 (LINEAR) � by Bernhard Haeusler, Germany

magnification 3x

The constitution of the dust/debris/boulder structure of P/2010 A2 should be more massive in comparison to the scattered material of desintegrating comets.
I.e. the end of C/1999 S4 (and probably the actual end of C/2009 O2 too) was going on very fast.

The next opposition of P/2010 A2 will occur in May/June 2011. This will be an interesting opportunity the take more images and to check,
 if the structure has changed. Maybe the Solar Wind will not disperse the destroyed material of the collided asteroids until next year.


MPC observation computed with Astrometrica  MPC2010-E50 of March, 12 2010

COD B82
OBS Bernhard Haeusler
TEL 0.30-m Schmidt-Cassegrain + CCD

NET CMC-14

PK10A020 KC2010 03 11.86046 06 51 59.13 +24 21 57.0 19.3 N B82
PK10A020 KC2010 03 11.87791 06 52 00.30 +24 21 50.6 18.9 N B82
PK10A020 KC2010 03 11.89534 06 52 01.09 +24 21 44.4 18.9 N B82

Gauss curve produced by Astrometrica. The total PSF is using the aperture circle of 3 x 3 pixel around the brightest pixel.
You see the Gauss curve right as the computed ideal line and the real pixels contributed around the ideal line.
The Fit RMS is the deviation from the ideal line (inlay under the Gauss curve).


Photometry computed with FOCAS II, using the Multibox method:

COD B82
OBS Bernhard Haeusler
CATALOG: USNO A2.0 / CMC-14 - BAND: R

                                                      10x10  20x20  30x30  40x40  50x50  60x60   SNR   SB  COD
OBJECT        DATE       TIME       +/-       +/-       +/-       +/-       +/-      +/-  N  FWHM  CAT
------------  ---------- --------  -----  -----  -----  -----  -----  -----  ----  ----  ---

P/2010 A2     11/03/2010 21:10:11 19.33 18.92 19.02 19.07 18.96 18.79 3.8 22.6 B82
P/2010 A2     11/03/2010 21:10:11* 0.17 0.23 0.23 0.24 0.35 0.40 5 5.6 CMC

FoCAs II - 07/01/2009-b

FOCAS II is a tool for photometry on the base of data coming from Astrometrica. Focas is basically using the .LOG file of Astrometrica.

Explanation of the FOCAS II table headings:

Object, date and time are self-explaining.
10x10, 20x20 ... 60x60 are the measured magnitudes according to the aperture sizes of photometry in arc sec (circle).
SNR is the  Signal-to-noise ratio for aperture photometry (calculator).
SB is the magnitude of the faintest star on the image matching with the used star catalogue. This is not the faintest star of the image!
COD is the MPC Code of the observatory.

second line:
+/- are the precisions of the measurements.
N is the number of the used images for the measurements.
FWHM is the Full-Width Half-Maximum of the total PSF: Measure of the seeing.
CAT is the used star catalog in Astrometrica. x


links:

http://astrosurf.com/cometas-obs/index_i.htm Visual and CCD Observations and images from the "Cometas Obs" mailing list, using the Focas II format

es.groups.yahoo.com/group/Cometas_Obs The Spanish comet observation group in Yahoo

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