There were six C flares and one M flare on the Sun during the past 24 hours, released by NOAA AR 11996 and 12003. The M1.2 flare was produced by NOAA AR 11996 and peaked at 19:19 UT on March 13. In the next 48 hours, the probability for C flares is very high (above 90%) and for M flares around 50%, mainly from NOAA AR 11996. An X flare is possible but unlikely. LASCO C2 imagery featured a CME starting at 10:00 UT on March 14 in the northeast to southeast. The same CME was spotted on COR2 A and COR2 B images in the northwest to southwest. This CME is most probably associated to a backside filament eruption, which was observed in EUVI B at about 9:36 UT. Hence, this CME will not be geoeffective.In the past 24 hours, solar wind speed as observed by ACE further rose from about 350 km/s to a plateau of about 520 km/s, while the magnitude of the Interplanetary Magnetic Field (IMF) varied between 2 and 10 nT. This is probably the effect of a southern coronal hole high speed stream. A small coronal hole at about 30N passed the central meridian on March 13. It may influence the geomagnetic field on March 17 and 18. In the past 24 hours, quiet geomagnetic levels were registered (K Dourbes between 0 and 2; NOAA Kp between 1 and 3). Quiet to active geomagnetic conditions (K Dourbes < 5) are expected on March 14 under the influence of the high speed stream. Quiet conditions (K Dourbes < 4) are likely on March 15 and 16. SIDC
NGC 2685 is a confirmed polar ring galaxy – a rare type of galaxy with stars, gas and dust orbiting in rings perpendicular to the plane of a flat galactic disk. The bizarre configuration could be caused by the chance capture of material from another galaxy by a disk galaxy, with the captured debris strung out in a rotating ring. Still, observed properties of NGC 2685 suggest that the rotating ring structure is remarkably old and stable. In this sharp view of the peculiar system also known as Arp 336 or the Helix galaxy, the strange, perpendicular rings are easy to trace as they pass in front of the galactic disk, along with other disturbed outer structures. NGC 2685 is about 50,000 light-years across and 40 million light-years away in the constellation Ursa Major.
Sharpless 132 is a faint emission nebula at the Cepheus/Lacerta border, it measures 42 x 30 arcminutes. It lies about a degree southeast of ε Cep. It can be glimpsed visually, but that takes a rich-field refractor and very dark skies. Sh2-132 lies in the field of the Cepheus OB1 association. It is related to Cep OB1, whose distance is given as 10,000 to 12,000 light-years, thus it is located in the Perseus arm of our Galaxy, and measures more than 250 light years in extent. Some photographers call it “The Lion Nebula” due to its shape (head upper left, tail to the right, four legs below). It features a conspicuous dark lane in the “head” section.
Imaging telescopes or lenses: Astro-Physics AP 130mm f/6.3 Starfire EDF
Imaging cameras: SBIG STXL-11002/FW8G-STXL
Mounts: Astro-Physics Mach1AP GTO with GTOCP3
Guiding telescopes or lenses: Astro-Physics AP 130mm f/6.3 Starfire EDF
Guiding cameras: SBIG STXL-11002/FW8G-STXL
Software: Pleiades Astrophoto Pixinsight 1.8, Photoshop CS5, Cyanogen Maxim DL Pro 5
Filters: Astrodon 3nm SII, Astrodon 3nm OIII
Dates: Oct. 14, 2013, Oct. 26, 2013, Oct. 27, 2013
Astrodon 3nm OIII: 14×900″ bin 1×1
Astrodon 3nm SII: 15×900″ bin 1×1
Astrodon H-alpha 3 nm: 25×900″ bin 1×1
Integration: 13.5 hours
14 March 2014
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