Pesquisando por: "About Schmidt" - Fotoarena - Agência de fotojornalismo

PIX4571830 The three stars that make up the Centaur Alpha System are the closest stars to the Sun. The image on the left shows the double alpha star of the Centauri (Alpha Centauri A and B) overexposed to the red dwarf star Proxima of the Centaurus (indicated by the arrow). Proxima du Centaur is located at a distance of 4.22 years - light from the Sun but is invisible to the naked eye. Alpha Centauri A and B are a little further away, 4.36 years from the Sun. These two stars are relatively similar to the Sun. Although Proxima of Centauri is distant from the Alpha couple of Centauri, its movement seems to link it to this system and is sometimes called Alpha Centauri C. Location of the Alpha Centauri triple stellar system in the sky. The brighter stars (Alpha Centauri A and B) are strongly overexposed, with the outlying member, Proxima lying approx. 2.2* to the south - west (arrow). Smaller areas around the stars are shown in the inserts to the right. The photo has been reproduced from a blue - sensitive photographic plate obtained by the ESO 1 - m Schmidt Telescope, a wide - angle telescope at the La Silla observatory in Chile that has now been decommissioned. The Alpha Centauri triple stellar system is our closest neighbour in space. It is located at a distance of 4.36 light - years, or 41 million km, in the direction of the southern constellation Centaurus (The Centaur). The two main stars in the system, Alpha Centauri A and Alpha Centauri B, are rather similar to the Sun; their stellar spectral types are “” G2V”” and “” K1V””, respectively. The third star is a “” red dwarf”” known as Proxima. It is much cooler and smaller than the other two. Alpha Centauri A and B orbit each other at a distance of about 3600 million km, or somewhat more than the distance of planet Uranus from the Sun. The orbital period is almost exactly 80 years. Their smaller companion, Proxima, is about

PIX4621421 Antares star and the nebula Rho Ophiuchi - Antares and Rho Ophiuchi cloud - This coloree nebula represents the visible part of a very large molecule cloud, the cloud of Ophiuchus. This star-forming region is about 520 years old - light. The brightest star at the bottom left is the star Antares, from the Scorpio. The triple star Rho Ophiuchus is located in the middle of the blue cloud at the top of the picture. On the right, surrounded by a nebula, the star Sigma Scorpii. The globular clusters M4 (at the bottom of the image) and NGC 6144 (near Antares) are also visible on this image obtained with the UK Schmidt telescope of 1.2m. This photograph shows a portion of a great swath of obscuring gas and dust in the constellations Ophiuchus and Scorpius, and illustrates what is probably the most colourful region in the entire sky. The almost garish colours are due to the brilliance and contrasting colours of the stars, by whose reflected light we see the dust clouds. Dominating the picture is the first - magnitude red supergiant star Antares, or Apha Scorpii. Because of its deep red colour the light reflected from the dust has a rich reddish hue, unusual among such reflection nebulae which are generally associated with bright bluish stars and normally have the appearance of the nebula surrounding Rho Ophiuchus (top). Clearly to be seen on this picture is the discolouring effect of the dust clouds on the stars and nebulae seen through them: the dust selectively absorbs the blue light leaving the obscured objects with a reddish - brown tinge. Also visible in this extraordinary photograph is the yellowish globular star cluster M4, at 5700 light years (9 times the distance of the foreground dust and stars) the nearest globular cluster to the Sun. Partly surrounding Sigma Scorpii at the right of the picture is a red emission nebula, completing the most comprehensive collection of nebular types ever seen in one photograph. There's also two globular clusters, one

PIX4610376 Spiral galaxy M81 in the Great Bear - Spiral galaxy M81 in Ursa Major - The spiral galaxy M81 is located 12 million years ago - light from Earth. Its arms are home to star-forming regions while its core is surrounded by much older yellow stars. In the background at the top, an irregular dwarf galaxy, Holmberg IX. This image obtained by a 50 cm amateur telescope, in February 2010 for 23 hours of poses, shows gas filaments whose origin is uncertain. Located about 12 million light - years from our planet, M81 (NGC 3031) together with M82 (NGC 3034), NGC 3077 and NGC 2976 forms one of the most iconic groups of interacting galaxies. The M81 group has also been the subject of many studies searching for and analyzing evidence of strong interactions among its components. In 1965, Halton Arp detected an unusual looping feature near M81 while examining photographic plates produced with the 48 - inch Schmidt on Mount Palomar. Traditionally, ARP's loop has been interpreted as a tail resulting from the tidal interaction between M81 and M82. However, since its discovery that explanation has been doubted by many researchers. Interestingly, the region of the sky containing the M81 group of galaxies is filled with Galactic cirrus and ARP's loop exhibits colors and emission properties similar to those observed in Galactic cirrus clouds. This optical image suggests that the light observed at optical wavelengths is a combination of emissions from: recent star forming regions situated near M81, the extended disk of M81 and scattered light from the same Galactic cirrus that is responsible for the bulk of the far infrared emissions. Although our observations cannot exclude the presence of some material stripped from the disk of M81 (NGC 3031) and/or M82 (NGC 3034) that is chance located in our line of sight to and far behind this intruiging structure, our findings suggest that ARP's Loop is situated between the observer and M81 (