Is this a trick question? Generally speaking helium lines only form at temperatures well above the cooler temperatures where molecular traits
can form (to be displayed spectroscopically). So, the implied contradiction is two opposing thermal conditions - hi temp vs low temp - or two traits, He vs say O2, which require two contradictory temp conditions. Anything else would generally require a rather exotic set of circumstances, as say with a mass ejection having outer coronal propoerties with temps high enough to be burning helium (in a thin shell), but spatially removed near the core of the event things have since cooled and might be showing a few molecular traits - a long slit cross sectional spectrum of the entire area might conceivably yield a merged spectrum showing seemingly contradictory (thermal) traits. Take stars c,d, and d in the Trapezium, for example. Each of these systems contains an O or B primary star with smaller K to M type companions; a long slit application which takes in the whole system may very well (well it will!) show seemingly contradictory traits. It is precisely mixes of such traits which define a spectroscopic binary. Yes?
Have I answered you question? I did the best I could! (laughing)
walking speed.
Sn = 1 Sn = S(n-1)+12*(n-1), where S-0 (the first term) = 1 *This only works for stellar numbers of base 6
On the earth (and planetary/stellar bodies) they are called latitudes and longitudes.
The stellar property with the greatest range in values is luminosity. Stars can vary dramatically in brightness, from extremely faint red dwarfs with luminosities significantly lower than the Sun to massive, luminous supergiants that can be millions of times brighter. This vast range reflects differences in stellar size, temperature, and evolutionary stage. Consequently, luminosity serves as a key indicator of a star's characteristics and lifecycle.
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Stellar temperature can be measured by analysing the spectrum of light that stars emit; shorter wavelengths correspond to higher temperatures.
A stellar nursery is usually called a molecular cloud. A nebula is a generic term for an interstellar cloud of dust, gas and plasma.
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Stellar spectra are graphs or visual representations of the intensity of light emitted by a star at different wavelengths. They provide information about the star's temperature, chemical composition, and motion towards or away from Earth. Studying stellar spectra is crucial for understanding the properties and evolution of stars.
The dark lines are absorption spectrum, the energy absorbed by Atoms in the atmosphere of the star. ================================ Fraunhofer's spectral lines.
A stellar nursery is a region in space where new stars are born. These nurseries are typically found within giant molecular clouds where gas and dust come together under gravity to form stars. It is a crucial stage in the life cycle of stars.
The birthplace of stars is called a stellar nursery or star-forming region. These regions are often found within interstellar clouds of gas and dust where gravitational forces cause these materials to collapse and form new stars.
"Stellar" means "related to a star", so you can use it in expressions such as "stellar wind", "stellar atmosphere", "stellar fusion", etc.
Stellar spectroscopes work by collecting radiation from an astronomical object. Studying the electromagnetic spectrum can allow you to work out its temperature, chemical composition and other characteristics.
Stars begintheir lives burning hydrogen and converting it to helium. If there are large amounts of helium in a stellar spectrum, it would indicate that the star has been making helium for a long time - hence age.
The Solar System formed from the gravitational collapse of a giant molecular cloud (Stellar Nursery) [See Link] about 4.6 billion years ago. The molecular cloud was probably several light-years across and could have birthed several stars
The submillimeter wavelength range, specifically around 1 millimeter, has been proven to be the most useful in studying star birth in dense molecular clouds. This range allows astronomers to peer through the dense dust clouds where stars are forming, revealing critical details about the early stages of star formation. By observing at submillimeter wavelengths, astronomers can study the cool dust and gas that are signatures of young stellar objects.