Location/ Date:

Eggersdorf und Zepernick, GER / 1.-2.-7.-8. August 2015

Telescope/ Lens:

10" f/4 ONTC Newton / Zeiss 110-750 

Mount:

Celestron CGE GPS

Camera:

Atik 383L+ / Atik 460exm

Exposure time:

8x1800" Astronomik Ha 6nm CCD

22x900" Baader Ha 7nm CCD

16x1800" Astronomik [OIII]

Total exposure:

17.5 hours

Description:

The star BD +60°2522 40 times as massive and one hundred thousend times higher as our sun has created this giant bubble of ionized gas with his enourmus power and his powerful stellar winds. The bubble extends to a diameter of 6 light years. These extremely powerful stars start their life with a mass 25 times higher as the mass of our sun at least. Their surface temperature is between 30,000 and 60,000 Kelvin and their stellar winds can reach  a speed as high as 1500 km per second. WR stars can lose two thirds of their mass in the last phase of their life. A star with 35 solar masses can end up with more than 10 solar masses before he blows up as a supernova.The special shape of the bubble is marking tho front edge of the Wolf-Rayet wind, the enormous wind of this WR class star travel with a speed of up to 9 million km per hour. The asymmetric shape of the babble in regards to BD +60° 2552 is caused by slight density differences in the surrounding gaseous matter. Also the bright arcs and small agglomerations at the surface of the bubble are caused by density variations of the matter. The prominet bright inner node sprwling along the western wall of the bubble is in fact the ionized edge of a larger cloud physically located outside the bubble. The Bubble Nebula is embedded in the HII region Sharpless 162 (S162). The whole object is located in the Perseus arm of the Milky Way Galaxy. The star BD +60°2522 40 times as massive and one hundred thousend times higher as our sun has created this giant bubble of ionized gas with his enourmus power and his powerful stellar winds. The bubble extends to a diameter of 6 light years. These extremely powerful stars start their life with a mass 25 times higher as the mass of our sun at least. Their surface temperature is between 30,000 and 60,000 Kelvin and their stellar winds can reach  a speed as high as 1500 km per second. WR stars can lose two thirds of their mass in the last phase of their life. A star with 35 solar masses can end up with more than 10 solar masses before he blows up as a supernova. The special shape of the bubble is marking tho front edge of the Wolf-Rayet wind, the enormous wind of this WR class star travel with a spoeed of upo to 9 million km per hour. The asymmetric shape of the babble in regards to BD +60° 2552 is caused by slight density differences in the surrounding gaseous matter. Also the bright arcs and small agglomerations at the surface of the bubble are caused by density variations of the matter. The prominet bright inner node sprwling along the western wall of the bubble is in fact the ionized edge of a larger cloud physically located outside the bubble. The Bubble Nebula is embedded in the HII region Sharpless 162 (S162). The whole object is located in the Perseus arm of the Milky Way Galaxy.

Image recording:

Frank Iwaszkiewicz, Nico Geisler

Image processing:

Frank Iwaszkiewicz, Nico Geisler