The weakest hydrogen line stars are classified as Class V in the Morgan-Keenan (MK) system of stellar classification. These stars have very weak or no hydrogen lines in their spectra, indicating low surface temperatures and the presence of strong molecular absorption bands. Class V stars are typically red or brown dwarf stars.
A dashed line represents a hydrogen bond because they are the weakest of the bonds.
The three stars in a line are known as Orion's Belt. They are named Alnitak, Alnilam, and Mintaka. These stars are part of the larger constellation Orion.
Nuclear Fusion in a Giant Star involves Helium being fused into a hydrogen shell that surrounds the core, and Nuclear Fusion in a Main-Sequence star involves Hydrogen being fused into Helium to produce Energy inside of the core.
hydrogen
The hydrogen line emission spectrum was discovered by physicists Johann Balmer, Johannes Rydberg, and Niels Bohr. They observed that hydrogen gas emitted specific wavelengths of light, which formed a distinct spectrum now known as the Balmer series.
A dashed line represents a hydrogen bond because they are the weakest of the bonds.
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A hydrogen cloud is a region in space where a significant amount of hydrogen gas is present. These clouds typically exist in interstellar space and are important for the formation of stars and galaxies. The hydrogen gas in these clouds can be ionized, which makes them visible in certain wavelengths, such as in the H-alpha emission line.
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Although all the hydrogen in the sun and the stars will eventually be converted to helium or heavier elements, there is likely to be plenty of hydrogen atoms in outer space. This answer assumes, in line with current cosmological theories, that the universe does not end in a big crunch.
Supernova [See Link] classifications are based on chemical composition, not time.They are classified according to the absorption lines of different chemical elements that appear in their spectra.The first element for a division is the presence or absence of a line caused by hydrogen. If a supernova's spectrum contains a line of hydrogen in the visual portion of the spectrum) it is classified Type II; otherwise it is Type I.
The Balmer lines are strong in medium-temperature stars because this temperature range is where hydrogen atoms are most abundant and have a higher probability of transitioning between energy levels, emitting light in the visible spectrum. In hot stars, the high temperature causes electrons to be in higher energy levels, making the transitions less likely to emit visible light. In cool stars, the lower temperature means that most hydrogen atoms are in their ground state, resulting in fewer transitions and weaker Balmer lines.
The H-alpha absorption line of hydrogen in the Sun is weak because hydrogen at that level is mainly ionized due to the high temperatures and pressures in the Sun's outer layers. This ionization state alters the energy levels of the electrons, reducing the number of transitions that can create the H-alpha line in absorption.
The dividing line is usually considered to be when the accretion process stops and the T tauri wind begins. This is probably approximately coincident with the beginning of lithium fusion (a T tauri star is not yet hot and dense enough for hydrogen fusion to start).
In a row means one after another on the same line. So "stars in a row" mean there are stars one after another all on the same line.
The three stars in a line are known as Orion's Belt. They are named Alnitak, Alnilam, and Mintaka. These stars are part of the larger constellation Orion.