INFO FROM SIDC – RWC BELGIUM 2014 Oct 13
There are only two sunspot groups currently visible on the solar disk, andno C flares occurred during the past 24 hours. In the next 48 hours,eruptive conditions (C flaring) are possible, especially from beta regionNOAA AR 2187. A bright CME was first seen in the SOHO LASCO C2 field ofview at 00:00 UT on October 13. It had an angular width of about 90 degreesand is probably associated with an eruption in a backside region close tothe west limb. This CME is not expected to be geoeffective.Over the last 24hours, solar wind speed observed by ACE was low and fluctuated betweenabout 310 and 340 km/s. The magnitude of the Interplanetary Magnetic Field(IMF) first varied between 4 and 8.5 nT, and jumped from 5.5 to 9 nT around5:45 UT on October 13, possibly due to an unidentified ICME structure. Overthe past 24 hours, geomagnetic conditions were quiet (K Dourbes between 1and 3; NOAA Kp between 1 and 2). Quiet geomagnetic levels (K Dourbes < 4)are expected on October 13, 14 and 15, with a slight chance for activelevels (K Dourbes = 4) in the early hours of October 14 in case theglancing blow of the CME from October 10 encounters the Earth.
INFO FROM SIDC – RWC BELGIUM 2014
The solar activity is low. The strongest of three C-class flares reportedduring last 24 hours was the C2.5 flare (peaked at 05:15 UT) on October 12.All three C-class flares originated from the NOAA AR 2187 which iscurrently situated close to the east solar limb. No Earth directed CMEswere observed in last 24 hours. The flaring activity at the C-class levelis possible, in particular from the NOAA AR 2187.The Earth is currentlyinside a slow solar wind with the speed of 340 km/s, and the interplanetarymagnetic field magnitude has the average value of about 4nT. We expectquiet to unsettled geomagnetic conditions to continue in the followinghours.
FAST WARNING ‘PRESTO’ MESSAGE from the SIDC (RWC-Belgium) 2014
The partial halo CME, first seen in the SOHO LASCO C2 field of view at 16:12 UT on October 10 was associated with the concurrent filament eruption (situated at about S30 W45) and long duration C3.0 flare (peaked at 16:47 UT). The CME had angular width of about 200 degrees and was propagating with the projected speed of about 400 km/s (as reported by the CACTUS software). The bulk of the CME mass was ejected south-west from the Sun-Earth line. The arrival of the glancing blow from the CME-driven shock wave is possible in the evening of October 14.
NGC 281 is an H II region in the constellation of Cassiopeia and part of the Perseus Spiral Arm. It includes the open cluster IC 1590, the multiple star HD 5005, and several Bok globules. Colloquially, NGC 281 is also known as the Pacman Nebula for its resemblance to the video game character.
The nebula was discovered in August 1883 by E. E. Barnard, who described it as “a large faint nebula, very diffuse.” The multiple star HD 5005, also called \beta1, was discovered by S. W. Burnham. It consists of an 8th-magnitude primary with four companions at distances between 1.4 and 15.7 seconds of arc.
Imaging telescopes or lenses: William Optics FLT 110 TEC
Imaging cameras: Atik 314L+
Mounts: Skywatcher EQ6 goto
Focal reducers: TMB Field Flattner for FLT
Filters: Baader Planetarium Ha 7nm, Baader Planetarium OIII, SII
Dates: Oct. 1, 2014
Locations: Observatoire “Le Pré des Étoiles”
Integration: 3.0 hours
Avg. Moon age: 6.54 days
Avg. Moon phase: 41.10%
RA center: 13.254 degrees
DEC center: 56.624 degrees
Pixel scale: 1.863 arcsec/pixel
Orientation: 92.443 degrees
Field radius: 0.439 degrees
Аuthor: Claude Roth
AstroPhotography of the day of SPONLI, 13.10.2014