Project 1999 - Are there any elements infered by spectroscopy that we haven't discovered on earth.

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Are there any elements infered by spectroscopy that we haven't discovered on earth.

However they absorb the light so we know they exist somewhere out there in the universe.

Like Iron is absorbing some of the light from a star and then another element that we don't have an example of...

like has anyone taken the time to sit down with the data and match it up backwards.

I don't even know how to ask google this question. I thought I would ask here first incase there are any actual erudites.

Because that would be badass. ***they always gloss over this in documentaries !

Technetium, element 43 is the only one I could discover within 30 seconds of research. I'm to lazy to continue but lol that is kinda cool !

I don't know if it was infered by spectroscopy tho.

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oooh it could have been !

Technetium stars belong to the classes M, MS, S, SC and C-N. They are most often variable stars of the long period variable types. Current research indicates that the presence of technetium in AGB stars occurs after some evolution and that a significant number of these stars do not exhibit the metal in their spectra.

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we may have discovered it through fission tho before we really got into astronomy !

Helium was discovered by spectroscopy !
https://armaghplanet.com/spectroscop...of-helium.html

that is kinda cool !

Quote:

In 1868 astronomer Jules Janssen observed a solar eclipse in India through a prism. He noticed a bright yellow spectral line emanating from solar prominences – giant storms erupting from the Sun. The line was unidentified. At first it was thought to come from the chemical element sodium since it was close by to two other bright lines arising from this element. The two lines of sodium were known as the D1 and D2 Fraunhofer lines, named after their discoverer. The unknown line was identified later that year by astronomer Norman Lockyer in a solar spectrum and he named it the D3 Fraunhofer line. He concluded it was caused by a new, unknown element. Lockyer named it Helios, after the Greek word for the Sun. Helium was then unknown, and in fact was not discovered on the Earth for another 27 years, until 1895.

Several fascinating properties of helium have been discovered in the ensuing years. The alpha particle, produced through radioactive decay, was found to be a helium nucleus. It is the most basic product of nuclear fusion in stars, as protons are turned into helium nuclei. Helium, when cooled to near absolute zero, is a liquid and has no viscosity, a phenomenon we call superfluidity.

neet****

not suprising we started chasing nuclear stuff not long after :p

Most of the heavier elements at the end of the periodic table undergo radioactive decay to become smaller atoms, very quickly, and don't actually exist in nature because of that. In other words, they're artificial elements which are lab synthesized. Most of them cannot even form naturally, even among megastars.

That is to say, every element above 92 cannot exist due to any natural causes within the known mechanics of the universe.

Elements above 118 already have placeholder names in the event of their successful manufacture (synthesis), and indeed these numbers are reserved up to element 300 but they don't exist, and we haven't figured out even how to synthesize them, as the math involved in theoretically synthesizing every element after 118 includes variables which suggest highly unpredictable outcomes with some elements perhaps not even being synthesizable at all.

Attachment 23128

The ratio of neutrons to protons as atomic number increases is not a linear relation.

For example, helium is typically assumed to have 2 electrons and two protons, and in most cases 2 neutrons, but there are species of helium with 1 neutron,

Meanwhile hydrogen has 1 proton 1 electron and 0 protons, but species of hydrogen we call deuterium, and tritium have 1 or 2 neutrons. Anyhow, as you go up the periodic table, which numbers each element by its number of protons, the amount of neutrons necessary to stabilize the atom varies. After 118 the correct combination of protons to neutrons which would cause the atom to exist in the band of stability becomes increasingly vague and the math of how each combination of proton to neutron coupling would decay (upwards or downwards with alpha beta or gamma decay) is unknown as well.

Quote:

Originally Posted by Botten (Post 3646283)

ya i kinda like this guy

he's got a little bit of the Sybok going on tho