The document discusses the evolution of stars from birth to death. Stars are born in cold clouds of interstellar gas and dust that collapse under mutual gravitation to form protostars. As pressure and temperature increase in the protostar's core due to gravitational contraction, hydrogen burning becomes possible and the star becomes visible, establishing thermal equilibrium. More massive stars reach this stage of maturity as main sequence stars in only a few thousand years, while less massive stars take millions of years. In later stages, aging stars expand as their cores contract and outer layers expand, becoming red giants with lower surface temperatures. Upon exhausting their fuel, less massive stars end as white dwarfs while more massive stars explode as supernovae, leaving behind neutron stars or
This is the 3rd and final version of an invitational powerpoint presention to encourage Astronomical League members to attend the League's first of many Dark Sky conferences at Bryce Canyon National Park. Enjoy!
This is the 3rd and final version of an invitational powerpoint presention to encourage Astronomical League members to attend the League's first of many Dark Sky conferences at Bryce Canyon National Park. Enjoy!
Stillwaters - a silent way to climatise telecom closetsjan klamer
stillwaters is an environmental way to climatise cabinets and small rooms, it is very energy efficient and silent.
It works by using water as medium and the earth as inert heat body
Stillwaters - a silent way to climatise telecom closetsjan klamer
stillwaters is an environmental way to climatise cabinets and small rooms, it is very energy efficient and silent.
It works by using water as medium and the earth as inert heat body
'A star is a luminous sphere of plasma held together by its own gravity. The nearest star to Earth is the Sun. Many other stars are visible to the naked eye from Earth during the night, appearing as a multitude of fixed luminous points in the sky due to their immense distance from Earth. Historically, the most prominent stars were grouped into constellations and asterisms, the brightest of which gained proper names. Astronomers have assembled star catalogues that identify the known stars and provide standardised stellar designations. However, most of the stars in the Universe, including all stars outside our galaxy, the Milky Way, are invisible to the naked eye from Earth. Indeed, most are invisible from Earth even through the most powerful telescopes.'
I need this essay checked for correctness a proofread and w.pdfadianantsolutions
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Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
Cancer cell metabolism: special Reference to Lactate PathwayAADYARAJPANDEY1
Normal Cell Metabolism:
Cellular respiration describes the series of steps that cells use to break down sugar and other chemicals to get the energy we need to function.
Energy is stored in the bonds of glucose and when glucose is broken down, much of that energy is released.
Cell utilize energy in the form of ATP.
The first step of respiration is called glycolysis. In a series of steps, glycolysis breaks glucose into two smaller molecules - a chemical called pyruvate. A small amount of ATP is formed during this process.
Most healthy cells continue the breakdown in a second process, called the Kreb's cycle. The Kreb's cycle allows cells to “burn” the pyruvates made in glycolysis to get more ATP.
The last step in the breakdown of glucose is called oxidative phosphorylation (Ox-Phos).
It takes place in specialized cell structures called mitochondria. This process produces a large amount of ATP. Importantly, cells need oxygen to complete oxidative phosphorylation.
If a cell completes only glycolysis, only 2 molecules of ATP are made per glucose. However, if the cell completes the entire respiration process (glycolysis - Kreb's - oxidative phosphorylation), about 36 molecules of ATP are created, giving it much more energy to use.
IN CANCER CELL:
Unlike healthy cells that "burn" the entire molecule of sugar to capture a large amount of energy as ATP, cancer cells are wasteful.
Cancer cells only partially break down sugar molecules. They overuse the first step of respiration, glycolysis. They frequently do not complete the second step, oxidative phosphorylation.
This results in only 2 molecules of ATP per each glucose molecule instead of the 36 or so ATPs healthy cells gain. As a result, cancer cells need to use a lot more sugar molecules to get enough energy to survive.
Unlike healthy cells that "burn" the entire molecule of sugar to capture a large amount of energy as ATP, cancer cells are wasteful.
Cancer cells only partially break down sugar molecules. They overuse the first step of respiration, glycolysis. They frequently do not complete the second step, oxidative phosphorylation.
This results in only 2 molecules of ATP per each glucose molecule instead of the 36 or so ATPs healthy cells gain. As a result, cancer cells need to use a lot more sugar molecules to get enough energy to survive.
introduction to WARBERG PHENOMENA:
WARBURG EFFECT Usually, cancer cells are highly glycolytic (glucose addiction) and take up more glucose than do normal cells from outside.
Otto Heinrich Warburg (; 8 October 1883 – 1 August 1970) In 1931 was awarded the Nobel Prize in Physiology for his "discovery of the nature and mode of action of the respiratory enzyme.
WARNBURG EFFECT : cancer cells under aerobic (well-oxygenated) conditions to metabolize glucose to lactate (aerobic glycolysis) is known as the Warburg effect. Warburg made the observation that tumor slices consume glucose and secrete lactate at a higher rate than normal tissues.
Richard's entangled aventures in wonderlandRichard Gill
Since the loophole-free Bell experiments of 2020 and the Nobel prizes in physics of 2022, critics of Bell's work have retreated to the fortress of super-determinism. Now, super-determinism is a derogatory word - it just means "determinism". Palmer, Hance and Hossenfelder argue that quantum mechanics and determinism are not incompatible, using a sophisticated mathematical construction based on a subtle thinning of allowed states and measurements in quantum mechanics, such that what is left appears to make Bell's argument fail, without altering the empirical predictions of quantum mechanics. I think however that it is a smoke screen, and the slogan "lost in math" comes to my mind. I will discuss some other recent disproofs of Bell's theorem using the language of causality based on causal graphs. Causal thinking is also central to law and justice. I will mention surprising connections to my work on serial killer nurse cases, in particular the Dutch case of Lucia de Berk and the current UK case of Lucy Letby.
A brief information about the SCOP protein database used in bioinformatics.
The Structural Classification of Proteins (SCOP) database is a comprehensive and authoritative resource for the structural and evolutionary relationships of proteins. It provides a detailed and curated classification of protein structures, grouping them into families, superfamilies, and folds based on their structural and sequence similarities.
3. STELLAR EVOLUTION
Mrs.P.Kanmani,M.Sc.M.Phil.,
Birth of a star
Stars are born in
cold clouds of
interstellar gas and
dust floating in
space called Nebula.
Mutual
Gravitation
Form centres of
condensations
called Protostars.
Centre of
Gravity
Pressure and
temperature
increases to a
point where
hydrogen burning
is possible.
4. STELLAR EVOLUTION
Mrs.P.Kanmani,M.Sc.M.Phil.,
The outpouring energy of a protostar creates enough pressure to stop
gravitational contraction.
A thermal equilibrium is established and temperature is sufficient to
shine and be visible.
At this stage the star is completely convective.
Birth of a star
5. STELLAR EVOLUTION
Mrs.P.Kanmani,M.Sc.M.Phil.,
Maturity
When the transfer of energy in the core of a protostar changes from
convection to radiation it becomes main sequence star.
Now the core temperature is high enough to start a nuclear reaction.
A massive or super massive star will form in a few thousand years
where as less massive star take a few million years.
6. STELLAR EVOLUTION
Mrs.P.Kanmani,M.Sc.M.Phil.,
Maturity
In the process of hydrogen burning helium is formed.
To maintain thermal equilibrium the liberated energy in the interior is
radiated from the surface.
Due to radiation the temperature rises and star becomes more and
more luminous.
7. STELLAR EVOLUTION
Mrs.P.Kanmani,M.Sc.M.Phil.,
Ageing Stars
The helium formed by fusion is collected at the centre where no
hydrogen is available for burning.
To maintain thermal equilibrium the core starts to contract and outer
layer expands outwards.
As the size increases the energy radiated per unit area of surface
decreases and temperature falls down to 3000 K to 4000 K.
9. STELLAR EVOLUTION
Mrs.P.Kanmani,M.Sc.M.Phil.,
Death of a Star
When the temperature of Helium core reaches 108 K helium nuclei start
fusing into carbon through triple alpha process.
The death of a star is determined by its mass.
