H II region

Big clouds of gas make new stars.

These clouds are very bright. They glow in the dark sky.

New stars live in these clouds. They are often blue. These hot stars send out bright light. This light hits the gas around them.

The light makes the gas glow. This creates a special place in space. These places can be very big. They can hold thousands of stars.

Some of these places look like clumps. Others look like long threads. They can be many shapes.

New stars can live for a short time. Soon, they blow the gas away. The cloud will go away too. It is a busy place for stars.

An H II region is a place in space filled with glowing gas.

The name H II means the gas is ionized. This happens when light from hot stars hits the gas. This light knocks parts off the atoms. This makes the gas glow brightly.

These regions often start in giant molecular clouds. These are big, cold clouds made of hydrogen. When these clouds collapse, new stars are born. Most of these stars are hot and blue. They live for only a few million years. These stars give off much ultraviolet light. This light creates the H II region.

These places can be very large. Some are hundreds of light-years across. They can hold thousands of stars. They can also look like clumps or long threads. Some parts look like dark blobs. We call these Bok globules. They are places where even more stars may form. Soon, the hot stars and big explosions blow the gas away. This ends the life of the region.

An H II region is a huge area of glowing gas in space. The name H II uses a Roman numeral for two. It means the hydrogen gas is ionized. This happens when light from very hot stars hits the gas. This light knocks parts off the hydrogen atoms. These parts are called free protons. This process makes the gas glow very brightly.

These regions are often found inside giant molecular clouds. These clouds are very cold and very dense. They are made mostly of molecular hydrogen.

How does an H II region form? It starts when a giant molecular cloud begins to collapse. This collapse can be triggered by shock waves or collisions. As the cloud breaks apart, new stars are born. The most massive stars become very hot and blue. These stars emit a lot of ultraviolet light. This light creates an ionization front that moves through the gas. This front sweeps through the cloud at supersonic speeds. Eventually, the pressure from the gas causes the region to expand.

Humans have studied these regions for a long time. Nicolas-Claude Fabri de Peiresc discovered the Orion Nebula in 1610. Later, William Herschel saw it in 1774. He called it an unformed fiery mist. In the 1800s, William and Mary Huggins used a spectroscope to study them. They saw special lines of light in the gas. At first, some thought a new element called nebulium existed. Later, Henry Norris Russell showed it was just a familiar element in a new state.

Every H II region has different sizes and shapes. Some are tiny, called ultra-compact regions. They might be only one light-year across. Other regions are giant and hundreds of light-years wide. The density can range from a few particles to a million particles per cubic centimeter. Some regions, like 30 Doradus, are huge. Others, like NGC 604 in the Triangulum Galaxy, are also very large.

These regions can hold tens of thousands of stars. They can also reach temperatures of 10,000 K.

You can think of an H II region as a star nursery. It is a place where many stars are born at once. However, the stars also help destroy their own nursery. The strong winds from massive stars push the gas away. Supernova explosions also blow the gas apart. This happens after only one or two million years. Even dark blobs called Bok globules are part of this. These dark objects are sites where more stars might form.

An H II region is a large area of interstellar atomic hydrogen that has become ionized. In astronomy, the Roman numeral II indicates that the hydrogen is singly-ionized. This means the atoms have lost an electron, leaving behind free protons. These regions are vital to our understanding of the universe. They serve as massive star nurseries where new stars are born. They are typically found within giant molecular clouds, which are cold and dense. By studying these regions in distant galaxies, scientists can determine the chemical composition and distance of those galaxies.

The birth of an H II region follows a specific sequence of physical events. It begins with a giant molecular cloud, or GMC, which is mostly molecular hydrogen. These clouds are very cold, often between 10 and 20 K. A collapse is triggered by shock waves, collisions between clouds, or magnetic interactions. As the cloud fragments and collapses, new stars begin to form. The most massive stars created are very hot and blue. These stars emit intense ultraviolet light, which creates an ionization front. This front sweeps through the surrounding gas at supersonic speeds. As the ionized gas expands, it eventually creates the distinct H II region.

H II regions vary significantly in their physical characteristics. They can be categorized by their size and density. Some are ultra-compact H II regions, or UCHII, which may be one light-year across or less. These small regions are very dense, containing over a million particles per cubic centimeter. Other regions are giant H II regions that span hundreds of light-years. The density in these larger regions can drop to just a few particles per cubic centimeter. The temperature of an H II region typically reaches about 10,000 K. They also possess weak magnetic fields, often measured in several nanoteslas.

Humans have studied these glowing clouds for centuries. The French observer Nicolas-Claude Fabri de Peiresc discovered the Orion Nebula in 1610. In 1774, William Herschel observed the same nebula and called it a "fiery mist." Later, William and Mary Huggins used spectroscopy to study nebulae. They noticed unique emission lines in the light from the Orion Nebula. Scientists once thought these lines belonged to a new element called nebulium. However, Henry Norris Russell later proved the lines were actually from familiar elements in unusual conditions. This discovery helped astronomers understand the true nature of ionized gas.

The scale of these regions is truly immense. A giant H II region can contain tens of thousands of stars. For example, 30 Doradus in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy are massive examples. The mass of these regions can range between 100 and 10^5 solar masses. While spiral galaxies like the Milky Way have H II regions concentrated in their spiral arms, irregular galaxies have them scattered chaotically. In contrast, elliptical galaxies almost never contain these ionized regions.

While they are called nurseries, H II regions are also places of destruction. The process of star formation is quite inefficient. Less than 10 percent of the gas in the region actually turns into stars. The remaining gas is pushed away by radiation pressure from the hot, young stars. The most massive stars also produce strong stellar winds. After only one to two million years, these stars may explode as supernovae. These explosions, along with stellar winds, eventually disperse the remaining gas. This process effectively destroys the nursery that created the stars.

Within these regions, we find fascinating structures like Bok globules. These are small, dark, circular or oval objects seen in silhouette. Bart Bok and E. F. Reilly identified them in the 1940s as potential sites for star formation. It was later confirmed in 1990 that these globules are indeed where stars are born. As the radiation from the H II region drives material away, it can actually squeeze these globules. This pressure might trigger one final burst of star formation. Additionally, the Hubble Space Telescope has found protoplanetary disks, or proplyds, in the Orion Nebula. These disks contain much of the matter needed to build planetary systems.