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Some results from observations with the 70cm telescope:


Click the images to see an enlarged high resolution version.

click to enlarge MU Cam

Light curves of the intermediate polar (see, e.g., the 'beginner's guide to CVs' at MSSL or the article in Wikipedia) MU Cam in several energy bands (X-ray (top panel), UV (second from top), optical (third from top), and in sub-bands of the full X-ray range). The optical data were obtained with the 70cm-telescope simultaneously to an observation with the X-ray satellite XMM-Newton.

A short explanation you find in an article in the XMM-Newton Image Gallery, where the object is referenced by one of its other names, 1RXSJ062518.2+733433.

Data obtained with the 70cm-telescope were used in several publications on this object:
Staude et al. 2007 (A&A, submitted),
Staude et al. 2006 (Proc. The X-ray Universe 2005, ESA SP-604, 307)
Staude et al. 2003 (A&A 406, 253).


click to enlarge Ernestina

Ernestina is a planetoid that was observed with the 70cm-telescope.

A movie showing it moving in front of the stars and a short explanation you find here.


click to enlarge M1 (Crab Nebula)

© B. Thinius (2001)

This is a picture of M1, the "Crab Nebula". It was observed on January, 17th 2001 in three wavelength bands (B, V, R). These single exposures were colored (R-band with red, V-band with green and B-band with blue) and put together.

The Crab Nebula is the remnant of a supernova, which was observed in 1054 A.D. It is at a distance of approx. 1500 pc (4900 light years) and has a diameter of ~2 pc. Its outer parts are expanding with 1100 km/s, its central star is a pulsar.

(more images taken by B. Thinius with the 70cm-telescope)


click to enlarge HU Aqr

Here light curves of the AM Herculis star (see the 'beginner's guide to CVs' at MSSL) HU Aqr, taken at different times, are shown.

Both light curves are scaled to the same flux, so that one can see how the shape of the light curve changes with the system's brightness. The brightness depends on the amount of matter, which is accreted by the white dwarf in a certain time. The upper panel shows a so-called 'high-state' (with a high accretion rate), while in the lower panel a 'low-state' is to be seen.

These data were used in Schwope et al. (2001).


click to enlarge M82

© B. Thinius (2001)

This is a picture of M82, a spiral galaxy which is seen "edge on" , i.e. perpendicular to the rotation axis. The luminous parts (hot gas clouds and stars) are strongly obscured by cold gas clouds and dust.

This coloured image is the sum of pictures taken in the blue, green and red spectral range. (Observed on May 2nd, 2001.)

(more images taken by B. Thinius with the 70cm-telescope)

click to enlarge click to enlarge V1309 Ori

These are eclipse light curves of the AM Herculis star V1309 Ori (RX J0515.41+0104.6), which has an orbital period of 7.98 h, the longest one of all known polars.

In both diagrams the upper panel shows the brightness of V1309 Ori around an eclipse. One sees that the luminosity drops nearly 2 magnitudes within 10 minutes, stays at this level for half an hour, and than rises more than 2 magnitudes.
These strong variations are caused by the cover of the accretion stream by the main sequence star. The white dwarf is not bright enough to be resolved in V-band light curves.

The next panel shows the observed brightness of a non-variable comparison star, which was used to correct the luminosity of V1309 Ori for the actual observing conditions. The third panel shows a non-variable star, brightness-corrected with the above panel, which is used for checking the quality of the flux correction. The forth panel shows the observed sky brightness, the fifth the observed size of the stars, which is a measure for the errors of the brightness determination.

These data were used to derive a more accurate ephemeris of this system (Staude, Schwope & Schwarz 2001, accepted).


click to enlarge RX J1015+05

This is a collection of optical and xray light curves of the AM Herculis-star RX J1015+05.

The observations at the AIP where deciding for the determination of the orbital period of 79.88 min.
(see Burwitz V. et al. 1996)


click to enlarge RXJ0203+29

The AM Herculis-system RXJ0203+29 was observed many times with the 70cm-telescope.

These observations were used for determination of the orbital period (4 hours, 36 minutes) and a main part of the Master thesis of Robert Schwarz and a following publication (Schwarz R. et al., 1998).


Last change 2007/02/15