As a result of preceding actions the File opening dialog box appears and user is suggested to open the file with observations (the file may be created for the first time). ... To see the list of files with desirable extension in chosen folder define the type of extension with the help of File type drop-down list at the bottom of the dialog box. ... The name of the file will appear in File name dialog box. ... In case you want to open the file with new name, type it in the File name dialog box. ...

Nickolai Copernic: "making the Sun stop, pushing the Earth". ... The aim of Copernic's investigations is improving the calculating schemes. ... In heliocentric system appeared an opportunity of calculating real proportions of Solar system using the radius of the Earth's orbits as an astronomical unit. Copernic's book "About Rotation of Celestial Bodies" contains a discription of astronomical devices as well as a new more exact catalogue of stable stars. ...

... Spherical aberration, coma, and astigmatism are also easily observed using the star test. ... Off-axis images are complex. ... Fig. ... Diffraction by a circular aperture as a function of defocus for no aberration Airy Disk 1 wave defocus Less than 1 wave defocus Fig. ... Diffraction by a circular aperture as a function of defocus for third-order spherical aberration Paraxial Focus Small distance inside paraxial focus Moderate distance from marginal focus Immediate neighborhood of marginal focus Fig...

... To avoid extensive numerical calculations in the statistical simulations, we treat the continuous evolution of each binary component as a sequence of a finite number of basic evolutionary states (for example, main sequence, red (super)giant, helium (Wolf-Rayet) star,     hot WD), in which stellar parameters significantly differ from each other. ... Figure 2: Schematic representation of the typical evolutionary track of a massive binary system with normal and compact star stages indicated. ...

. Inbound . Outbound . AE8 . Previous slide . Next slide . Back to first slide . View graphic version .

... Circumstellar disc of beta Pictoris: constraints on grain properties from polarization. To appear in the Astronomy & Astrophysics . abs , src , ps ] . ... Dust influx to Titan from Hyperion . ... abs ] . ... Characteristics of bulges and disks in interacting galaxies . ... Dust grains around Herbig Ae/Be stars: porous, cometary-like grains? ... To appear in the Astronomy & Astrophysics Supplement . ... Finally, Links may lead you to more options (e.g. via the LANL preprint system). ...

UNIXhelp is available for anybody to use on the World Wide Web . However if you are based outside Edinburgh, you may find each page slow to load across the network. We would recommend installing a copy at your local site. ... The main distribution site appears below but there may be an mirror of the distribution closer to you. ... Contact the UNIXhelp maintainer if you can help. The Copyright for the UNIXhelp deliverables rests with the Computing Services of the University of Edinburgh. ...

The multiscale analysis of heterogeneous structures is actually an important and effective tool of mathematical modeling in physics, technique and biology. ... The special year will extend the existing cooperation between French and Russian researchers in the multiscale analysis and in mathematical modeling in hemodynamics, taking into consideration the mass transport, coagulation, fluid-structure interaction and other aspects. ...

... A pixmap is an off-screen buffer you can draw graphics into. After drawing into a pixmap, you can copy it to a window, causing it to appear on the screen (when the window is visible). ... In GDK, the pixmap type is called GdkPixmap . ... Drawables include windows, pixmaps, and bitmaps. ... GdkDrawable is used in function declarations when either a window or a pixmap is an acceptable argument. ... GdkPixmap* gdk_pixmap_new (GdkWindow* window , gint width , gint height , gint depth ); . ...

This widget allows you to adjust the secondary mirror focus. The seconary focus is actually an offset to the secondary mirror piston computed by the TCC (as it tries to compensate for changing temperature and altitude). ... Set... : set a new absolute secondary focus. ... XX and + XX buttons: offset the secondary focus by the amount shown. The mirror is moved as soon as you release the button. Increment Menu (25/50/100) : set the increment shown on the - XX and + XX buttons. ...

... 1st Announcement IAU Symposium 312 Star Clusters and Black Holes Across Cosmic Time, Beijing, China, Aug. 25-29, 2014 . ... SUBJECT: 1st Announcement IAU Symposium 312 Star Clusters and Black Holes Across Cosmic Time, Beijing, China, Aug. 25-29, 2014 . ... which will be held in Beijing, P.R. China, from August 25-29, 2014, hosted by Chinese Academy of Sciences . ... China), . ... 1st Announcement IAU Symposium 312 Star Clusters and Black Holes Across Cosmic Time, Beijing, China, Aug. ...

... click image to view discuss) . ... This is a quick shot of the near-Earth asteroid 2005 YU55 using four consecutive exposures from the Harvard MicroObservatory robotic telescope in Amado, Arizona, on the night of Nov. ... 10, 2015 . This is Comet Lovejoy C/2014 Q2 as it appeared at about 10:30 pm Saturday, Jan. 10, 2015, from my back yard in Belmont, MA, about 5 miles west of downtown Boston. ... Main image: 0.6 second exposure. ... Copyright (c) Amateur Telescope Makers of Boston, Inc. ...

July 19, 1998 . ... An example of the EUV large-scale chain revealed by the modified TRACE EUV images. The TRACE EUV (171 A) image of July 19, 1998 with a number of complicated chains and threads. In particular, an "8"-like structure appear to be present at the central area of the disc restricted by points 1-2-3-4. Some fragments of this structure consist of the two parallel threads. ... Back to the page of the TRACE chains . Back to the parent page . Last update: 9 August 1998 . ...

... Astrophysics Group . ... AMI Science . ... Observations of galaxy clusters are central to the AMI science programme. The AMI Small Array is used to observe already-known clusters with high-sensitivity and resolution, allowing us to extract detailed information about individual clusters and to build up statistics about the cluster population. ... Observing galaxy clusters at 15 GHz is tricky because of the contamination from foreground radio sources, which is where the Large Array comes in! ...