Stellar Radiation and the Nature of the Universe

OLIVER LODGE

doi:10.1038/121711c0

Stellar Radiation and the Nature of the Universe

Nature ◽

10.1038/121749c0 ◽

1928 ◽

Vol 121 (3054) ◽

pp. 749-749

Author(s):

W. W. L.

Keyword(s):

Stellar Radiation ◽

The Universe

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From Gas to Stars Over Cosmic Time

Science ◽

10.1126/science.1229229 ◽

2013 ◽

Vol 340 (6140) ◽

pp. 1229229 ◽

Cited By ~ 5

Author(s):

Mordecai-Mark Mac Low

Keyword(s):

Star Formation ◽

Star Formation Rate ◽

Formation Rate ◽

Cosmic Time ◽

First Stars ◽

Initial Rise ◽

Stellar Radiation ◽

History Of ◽

Supernova Explosions ◽

The Universe

From the time the first stars formed over 13 billion years ago to the present, star formation has had an unexpectedly dynamic history. At first, the star-formation rate density increased dramatically, reaching a peak 10 billion years ago of more than 10 times the present-day value. Observations of the initial rise in star formation remain difficult, poorly constraining it. Theoretical modeling has trouble predicting this history because of the difficulty in following the feedback of energy from stellar radiation and supernova explosions into the gas from which further stars form. Observations from the ground and space with the next generation of instruments should reveal the full history of star formation in the universe, and simulations appear poised to accurately predict the observed history.

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The Expansion of the Universe

International Journal of Scientific Research and Management ◽

10.18535/ijsrm/v8i07.aa01 ◽

2020 ◽

Vol 8 (07) ◽

pp. 25-31

Author(s):

Dr. Andreas Gimsa

Keyword(s):

Background Radiation ◽

Expanding Universe ◽

Stellar Radiation ◽

Expansion Of The Universe ◽

Accelerated Growth ◽

The Universe ◽

Physical Quantities

The expansion of the universe is explained, calculated and graphically displayed. The 3K background radiation is examined and interpreted as reflected and distributed stellar radiation. The role of entropy in cosmology is discussed. In our expanding universe it must remain constant. Physical quantities previously assumed to be constant are worked out to be variable. It is explained why the measured redshift is not due to an accelerated growth of the universe.

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An evolving photoelectric efficiency at cosmic noon?

Proceedings of the International Astronomical Union ◽

10.1017/s1743921319008925 ◽

2019 ◽

Vol 15 (S352) ◽

pp. 243-245

Author(s):

Jed McKinney ◽

Alexandra Pope ◽

Lee Armus ◽

Ranga Chary ◽

Mark Dickinson ◽

...

Keyword(s):

Fine Structure ◽

Polycyclic Aromatic Hydrocarbon ◽

Starburst Galaxy ◽

Heating And Cooling ◽

Stellar Radiation ◽

Gas Heating ◽

Polycyclic Aromatic ◽

Dust Component ◽

Mass Assembly ◽

The Universe

AbstractTo sustain star formation rates (SFRs) of hundreds to thousands of solar masses per year over millions of years, a galaxy must efficiently cool its gas. At z ∼ 2, the peak epoch for stellar mass assembly, tracers of gas heating and cooling remain largely unexplored. For one z ∼ 2 starburst galaxy GS IRS20, we present Spitzer IRS spectroscopy of Polycyclic Aromatic Hydrocarbon (PAH) emission, and ALMA observations of [C II] 158 μm fine-structure emission which we use to probe ISM heating/cooling. Coupled with an unusually warm dust component, the ratio of [C II] /PAH emission suggests a low photolelectric efficiency, and/or the importance of cooling from other far-IR lines in this galaxy. A low photoelectric efficiency at z ∼ 2 could be key for the peak in the SFR density of the universe by decoupling stellar radiation from ISM gas temperatures.

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