This document provides an overview of spectroscopy and how it can be used to determine the composition of astronomical objects. It discusses how light interacts with matter on an atomic level, causing absorption and emission spectra that act as "elemental barcodes." The spectra are caused by electrons transitioning between quantized energy levels in atoms and emitting or absorbing photons of specific wavelengths. Measuring the absorption lines in a star's spectrum allows astronomers to identify the elements present in a star's atmosphere and determine its chemical composition, such as the fact that hydrogen and helium make up over 97% of the Sun's mass.
Quantum Physics is already a very interesting subject, and so even though the presentation has all the required information to get yourself a hold on the subject, I would highly recommend everyone to do some extensive research. Well actually, there is no need for anyone to point out on the research part, you will automatically find yourselves filling the search history with some deep quantum-ish.
Planck's Quantum Theory and Discovery of X-raysSidra Javed
Planck's quantum theory
Discovery of X-rays and explanation of production of X-rays, relation between atomic number and frequency of X-rays, application and uses of X-rays.
Quantum Physics is already a very interesting subject, and so even though the presentation has all the required information to get yourself a hold on the subject, I would highly recommend everyone to do some extensive research. Well actually, there is no need for anyone to point out on the research part, you will automatically find yourselves filling the search history with some deep quantum-ish.
Planck's Quantum Theory and Discovery of X-raysSidra Javed
Planck's quantum theory
Discovery of X-rays and explanation of production of X-rays, relation between atomic number and frequency of X-rays, application and uses of X-rays.
These notes covers chemistry chapter 2nd of class 11th which are strictly according to CBSE & state board syllabus.The contents covered are Model of atom, electronic configuration & many more..
The Roman Empire A Historical Colossus.pdfkaushalkr1407
The Roman Empire, a vast and enduring power, stands as one of history's most remarkable civilizations, leaving an indelible imprint on the world. It emerged from the Roman Republic, transitioning into an imperial powerhouse under the leadership of Augustus Caesar in 27 BCE. This transformation marked the beginning of an era defined by unprecedented territorial expansion, architectural marvels, and profound cultural influence.
The empire's roots lie in the city of Rome, founded, according to legend, by Romulus in 753 BCE. Over centuries, Rome evolved from a small settlement to a formidable republic, characterized by a complex political system with elected officials and checks on power. However, internal strife, class conflicts, and military ambitions paved the way for the end of the Republic. Julius Caesar’s dictatorship and subsequent assassination in 44 BCE created a power vacuum, leading to a civil war. Octavian, later Augustus, emerged victorious, heralding the Roman Empire’s birth.
Under Augustus, the empire experienced the Pax Romana, a 200-year period of relative peace and stability. Augustus reformed the military, established efficient administrative systems, and initiated grand construction projects. The empire's borders expanded, encompassing territories from Britain to Egypt and from Spain to the Euphrates. Roman legions, renowned for their discipline and engineering prowess, secured and maintained these vast territories, building roads, fortifications, and cities that facilitated control and integration.
The Roman Empire’s society was hierarchical, with a rigid class system. At the top were the patricians, wealthy elites who held significant political power. Below them were the plebeians, free citizens with limited political influence, and the vast numbers of slaves who formed the backbone of the economy. The family unit was central, governed by the paterfamilias, the male head who held absolute authority.
Culturally, the Romans were eclectic, absorbing and adapting elements from the civilizations they encountered, particularly the Greeks. Roman art, literature, and philosophy reflected this synthesis, creating a rich cultural tapestry. Latin, the Roman language, became the lingua franca of the Western world, influencing numerous modern languages.
Roman architecture and engineering achievements were monumental. They perfected the arch, vault, and dome, constructing enduring structures like the Colosseum, Pantheon, and aqueducts. These engineering marvels not only showcased Roman ingenuity but also served practical purposes, from public entertainment to water supply.
How to Make a Field invisible in Odoo 17Celine George
It is possible to hide or invisible some fields in odoo. Commonly using “invisible” attribute in the field definition to invisible the fields. This slide will show how to make a field invisible in odoo 17.
We all have good and bad thoughts from time to time and situation to situation. We are bombarded daily with spiraling thoughts(both negative and positive) creating all-consuming feel , making us difficult to manage with associated suffering. Good thoughts are like our Mob Signal (Positive thought) amidst noise(negative thought) in the atmosphere. Negative thoughts like noise outweigh positive thoughts. These thoughts often create unwanted confusion, trouble, stress and frustration in our mind as well as chaos in our physical world. Negative thoughts are also known as “distorted thinking”.
How to Create Map Views in the Odoo 17 ERPCeline George
The map views are useful for providing a geographical representation of data. They allow users to visualize and analyze the data in a more intuitive manner.
The Indian economy is classified into different sectors to simplify the analysis and understanding of economic activities. For Class 10, it's essential to grasp the sectors of the Indian economy, understand their characteristics, and recognize their importance. This guide will provide detailed notes on the Sectors of the Indian Economy Class 10, using specific long-tail keywords to enhance comprehension.
For more information, visit-www.vavaclasses.com
The French Revolution, which began in 1789, was a period of radical social and political upheaval in France. It marked the decline of absolute monarchies, the rise of secular and democratic republics, and the eventual rise of Napoleon Bonaparte. This revolutionary period is crucial in understanding the transition from feudalism to modernity in Europe.
For more information, visit-www.vavaclasses.com
Model Attribute Check Company Auto PropertyCeline George
In Odoo, the multi-company feature allows you to manage multiple companies within a single Odoo database instance. Each company can have its own configurations while still sharing common resources such as products, customers, and suppliers.
Operation “Blue Star” is the only event in the history of Independent India where the state went into war with its own people. Even after about 40 years it is not clear if it was culmination of states anger over people of the region, a political game of power or start of dictatorial chapter in the democratic setup.
The people of Punjab felt alienated from main stream due to denial of their just demands during a long democratic struggle since independence. As it happen all over the word, it led to militant struggle with great loss of lives of military, police and civilian personnel. Killing of Indira Gandhi and massacre of innocent Sikhs in Delhi and other India cities was also associated with this movement.
Palestine last event orientationfvgnh .pptxRaedMohamed3
An EFL lesson about the current events in Palestine. It is intended to be for intermediate students who wish to increase their listening skills through a short lesson in power point.
2024.06.01 Introducing a competency framework for languag learning materials ...Sandy Millin
http://sandymillin.wordpress.com/iateflwebinar2024
Published classroom materials form the basis of syllabuses, drive teacher professional development, and have a potentially huge influence on learners, teachers and education systems. All teachers also create their own materials, whether a few sentences on a blackboard, a highly-structured fully-realised online course, or anything in between. Despite this, the knowledge and skills needed to create effective language learning materials are rarely part of teacher training, and are mostly learnt by trial and error.
Knowledge and skills frameworks, generally called competency frameworks, for ELT teachers, trainers and managers have existed for a few years now. However, until I created one for my MA dissertation, there wasn’t one drawing together what we need to know and do to be able to effectively produce language learning materials.
This webinar will introduce you to my framework, highlighting the key competencies I identified from my research. It will also show how anybody involved in language teaching (any language, not just English!), teacher training, managing schools or developing language learning materials can benefit from using the framework.
3. The Nature of Light
The electromagnetic (EM) wave
A small disturbance in an electric
field creates a small magnetic field,
which in turn creates a small electric
field and so on…
EM waves transport energy.
Particles of light (photons)
travel through space.
These photons have very
specific energies, that is,
light is quantized.
• Light is radiant energy.
• Travels very fast –
300,000 km/sec!
• Light can be described
as either a wave or a
particle.
4. The Effect of Distance on Light
• Light from distant objects
seems very dim
• Why? Because the photons are
losing energy?
• No – because the light is simply
spreading out as it travels from
its source to its destination.
• The farther from the source
you are, the dimmer the light
seems.
• We say that the object’s
brightness or amount of light
received from a source is
decreasing.
2
d4
OutputLightTotal
Brightness
This is an inverse-square law –
the brightness decreases as the
square of the distance (d) from
the source increases.
5. The Nature of Matter
• The atom has a nucleus at its
center containing protons
and neutrons.
• Outside of the nucleus,
electrons whiz around in
clouds called orbitals
– Electrons can also be
described using wave or
particle models
– Electron orbitals are
quantized – that is, they
exist only at particular
energies.
– The lowest energy orbital
is called the ground state,
one electron wave long.
• To move an electron from one orbital to the
next higher, a specific amount of energy
must be added. Likewise, a specific
amount of energy must be released for an
electron to move to a lower orbital.
• These are called electronic transitions.
Please insert figure 21.3
6. The Chemical Elements
• The number of protons (atomic number) in the
nucleus determines which element a substance is.
• Each element has a number of electrons equal to the
number of protons.
• The electron orbitals are different for each element,
and the energy differences between the orbitals are
unique as well.
• This means that if we can detect the energy emitted
or absorbed by an atom during an electronic
transition, we can tell which element the atom
belongs to, even from millions of light years away!
7. Absorption
• If a photon of exactly
the right energy
(corresponding to the
energy difference
between orbitals) strikes
an electron, that
electron will absorb the
photon and move into
the next higher orbital
– The atom is now in an
excited state
• If the photon is of
higher or lower
energies, it will not be
absorbed – it will pass
through as if the atom
were not there.
• This process is called absorption
• If the electron gains enough energy
to leave the atom entirely, we say the
atom is now ionized. It is an ion.
Please insert figure 21.6
8. Emission
• If an atom drops
from one orbital
to the next lower
one, it must first
emit a photon
with the same
amount of energy
as the orbital
energy difference.
• This is called
emission.
Please insert figure 21.4
9. Seeing Spectra
http://www.youtube.com/watch?v=QI50GBUJ48s
• Seeing the Sun’s
spectrum requires a
few special tools, but
it is not difficult.
• A narrow slit only lets a
little light into the
experiment.
• Either a diffraction
grating or a prism splits
the light into its
component colors.
• If we look closely at the
spectrum, we can see
lines, corresponding to
wavelengths of light that
were absorbed.
10. The Bohr Model:
http://www.youtube.com/watch?v=45KGS1Ro-sc
• The Danish physicist Niels Bohr developed a model of the hydrogen
in the early 1900s that describes its possible energy levels.
• The Bohr model of hydrogen describes the electron as orbiting at a set
of discrete radii.
• If we number the energy levels starting from the ground state as n = 1,
2, 3 and so on, then the electron’s orbital radius is r = 0.053 × n2
nanometers (nm). (1 nm = 10−9 m).
• The energy En of level n can be described by the formula:
E1 (Hydrogen) = - 2.18 x 10-18 J/n2 = -13.6 eV/n2
n = 1 is the ground state quantum number and E1 is the ground
state energy.
1 eV = 1.60 x 10-19 J
11. Hydrogen Energy Levels
E1 = -13.6 eV/12 = -13.6 eV
E2 = -13.6 eV/22 = -3.4 eV
E3 = -13.6 eV/32 = -1.5 eV
E4 = …
.
.
E∞ = 0
12. Emission Spectra
http://www.youtube.com/watch?v=8TJ2GlWSPxI&feature=related
• Imagine that we heat up a
gas of atoms.
• Collisions among the atoms
cause electrons to jump to
higher orbitals, hence higher
energy levels.
• Collisions can also cause the
electrons to fall to lower levels,
emitting photons of energy:
E = hυ = hc/.
• If the electron falls from
orbitals 3 to 2 in hydrogen, the
emitted photon will have a
wavelength of = 656 nm. Red
• If the electron falls from orbital
4 to orbital 2, the emitted
photon will have a wavelength
of = 486 nm. Blue
• We can monitor the gas, counting the number
of photons at each wavelength. If we graph
this data, we’ll see an emission spectrum.
13. Emission spectrum of hydrogen
http://csep10.phys.utk.edu/astr162/lect/light/absorption.html
http://www.youtube.com/watch?v=OJzW2RoZq1Y&feature=related
14. Atomic Spectra: Elemental Fingerprint
• Every element has its own
spectrum. A fingerprint so to
speak. Note the differences
between hydrogen and helium
spectra below.
15. Absorption
Spectra
• What if, instead of hot
hydrogen gas, we had a
cloud of cool gas between
us and a star?
• Photons of an energy that
corresponds to the
electronics transitions in
hydrogen will be
absorbed by electrons in
the gas.
• The light from these
photons is effectively
removed from the
spectrum.
• The spectrum will have
dark lines where the
missing light would be:
An Absorption Spectrum:
The elemental barcode!
16. Types of Spectra
• Kirchoff’s Laws:
– If the source emits light that is
continuous and all colors are
present, we say that this is a
continuous spectrum.
– If the gas molecules are moving
rapidly (i.e., high temperature),
the atoms will emit characteristic
frequencies of light. This is an
emission-line spectrum.
– If the molecules of gas are cool,
they will absorb light of a
characteristic frequency as it
passes through. This is an
absorption line spectrum.