But what am I going to see? I don't know. In a certain sense, it depends on you.


H2 Region - LAST UNITS!.
H2 Region - LAST UNITS!.
H2 Region - LAST UNITS!.
H2 Region - LAST UNITS!.
H2 Region - LAST UNITS!.

Der Zyklus H2 Region - LAST UNITS!

Fundamental Records ONE by ONE
FR012-9
2 Tracks


Limited Edition 12"
Smoke Ultra-Clear Record Silkscreen Printed Glow in The Dark - LAST UNITS!!

Sold Out 24,99 29,99
H2 Region - LAST UNITS!.
H2 Region - LAST UNITS!.
H2 Region - LAST UNITS!.
H2 Region - LAST UNITS!.

 FUNDAMENTAL RECORDS ONE by ONE 

This record is part of the Time Capsule project aka 808 Box. Every time we manufacture a project with so many different records the manufacture plant always send more or less copies of some records but only a few times the exact amount. This is a spare copy, a leftover, but new and unplayed as the copies included in the limited edition boxes.

Now for first time all these records are available at our store. For the people who missed the opportunity to buy the full box is now or never, also for some of you who were only interested in some of them and not the full box. 

All Tracks Mastered by Alek Stark

 

ABOUT H II REGION by DER ZYKLUS

Extra 12" record by Der Zyklus included in the third 808 Box.

12" in 180gr. Smoke marbled in ultra clear compound, silkscreen printed with glow in dark ink.

Includes a second track, an alternative version by Alek Stark

CONCEPT

An H II region or HII region is a region of interstellar atomic hydrogen that is ionized. It is typically a cloud of partially ionized gas in which star formation has recently taken place, with a size ranging from one to hundreds of light years, and density from a few to about a million particles per cubic cm. The Orion Nebula, now known to be an H II region, was observed in 1610 by Nicolas-Claude Fabri de Peiresc by telescope, the first such object discovered.

H II regions can be observed at considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In spiral galaxies, including our Milky Way, H II regions are concentrated in the spiral arms, while in irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.

An HI region or H I region is a cloud in the interstellar medium composed of neutral atomic hydrogen (HI), in addition to the local abundance of helium and other elements. These regions do not emit detectable visible light (except in spectral lines from elements other than hydrogen) but are observed by the 21-cm (1,420 MHz) region spectral line. This line has a very low transition probability, so requires large amounts of hydrogen gas for it to be seen. At ionization fronts, where HI regions collide with expanding ionized gas (such as an H II region), the latter glows brighter than it otherwise would. The degree of ionization in an HI region is very small at around 10−4 (i.e. one particle in 10,000). At typical interstellar pressures in galaxies like the Milky Way, HI regions are most stable at temperatures of either below 100 K or above several thousand K; gas between these temperatures heats or cools very quickly to reach one of the stable temperature regimes. Within one of these phases, the gas is usually considered isothermal, except near an expanding H II region. Near an expanding H II region is a dense HI region, separated from the undisturbed HI region by a shock front and from the H II region by an ionization front.

 FUNDAMENTAL RECORDS ONE by ONE 

This record is part of the Time Capsule project aka 808 Box. Every time we manufacture a project with so many different records the manufacture plant always send more or less copies of some records but only a few times the exact amount. This is a spare copy, a leftover, but new and unplayed as the copies included in the limited edition boxes.

Now for first time all these records are available at our store. For the people who missed the opportunity to buy the full box is now or never, also for some of you who were only interested in some of them and not the full box. 

All Tracks Mastered by Alek Stark

 

ABOUT H II REGION by DER ZYKLUS

Extra 12" record by Der Zyklus included in the third 808 Box.

12" in 180gr. Smoke marbled in ultra clear compound, silkscreen printed with glow in dark ink.

Includes a second track, an alternative version by Alek Stark

CONCEPT

An H II region or HII region is a region of interstellar atomic hydrogen that is ionized. It is typically a cloud of partially ionized gas in which star formation has recently taken place, with a size ranging from one to hundreds of light years, and density from a few to about a million particles per cubic cm. The Orion Nebula, now known to be an H II region, was observed in 1610 by Nicolas-Claude Fabri de Peiresc by telescope, the first such object discovered.

H II regions can be observed at considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In spiral galaxies, including our Milky Way, H II regions are concentrated in the spiral arms, while in irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.

An HI region or H I region is a cloud in the interstellar medium composed of neutral atomic hydrogen (HI), in addition to the local abundance of helium and other elements. These regions do not emit detectable visible light (except in spectral lines from elements other than hydrogen) but are observed by the 21-cm (1,420 MHz) region spectral line. This line has a very low transition probability, so requires large amounts of hydrogen gas for it to be seen. At ionization fronts, where HI regions collide with expanding ionized gas (such as an H II region), the latter glows brighter than it otherwise would. The degree of ionization in an HI region is very small at around 10−4 (i.e. one particle in 10,000). At typical interstellar pressures in galaxies like the Milky Way, HI regions are most stable at temperatures of either below 100 K or above several thousand K; gas between these temperatures heats or cools very quickly to reach one of the stable temperature regimes. Within one of these phases, the gas is usually considered isothermal, except near an expanding H II region. Near an expanding H II region is a dense HI region, separated from the undisturbed HI region by a shock front and from the H II region by an ionization front.

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