The Chronological Life of Christ part 097 (Reality Check Luke 13 1-9).pptx
The solar wind2.pptx
1. The Solar Wind
By Feliks Rogotskiy
Ardrey Kell High School
Charlotte, NC 2023
https://www.linkedin.com/in/feliks-rogotskiy-
351874280/
2. The Sun
Sun consists mainly of hydrogen (71% by mass)
and helium (27% by mass). State – plasma. The
outer atmosphere of the Sun is known as the
corona.
The Sun rotates on its axis once in about 27 days.
Since the Sun is a ball of gas/plasma, The Sun’s
equator rotates more rapidly than its polar regions –
once every 24 days at the equator and once every
35 days at the poles.
The source of this "differential rotation" is an area
of current research in solar astronomy.
3. Space Weather
“Space weather” is measured by the:
● Speed
● Pressure and density of the solar wind
● Types of electromagnetic radiation bombarding the Earth’s upper
atmosphere
● Extent and interaction of the Earth’s magnetic field with that of the
solar wind.
Within the sun’s atmosphere, streams of charged particles get heated
to the point where gravity can’t hold them inside the atmosphere.
These charged particles then move along the sun’s magnetic field,
which is created as charged particles move around inside the sun.
This magnetic field is very large and spreads out all over the solar
system. The solar wind pushing on Earth's magnetic field.
4.
5. What is the solar wind?
The solar wind is primarily composed of roughly equal
numbers of protons and electrons, as well as a few
heavier ions.
Solar wind moves along magnetic fields. Solar wind
passes by Earth.
Deep Space Climate Observatory (DSCOVR) is an
American space weather station that monitors changes in
the solar wind, providing space weather alerts and
forecasts for geomagnetic storms that could disrupt
power grids, satellites, telecommunications, aviation and
GPS.
7. The Solar Wind Effects
Solar wind protects us from cosmic rays from other places.
Earth’s magnetic field protects us from solar wind.
Magnetic field redirects solar wind to the poles.
8. A coronal mass ejection (CME)
Coronal mass ejections (CMEs) are large expulsions of
plasma and magnetic field from the sun's atmosphere — the
corona.
Compared to solar flares — bursts of electromagnetic
radiation that travel at the speed of light, reaching Earth in just
over 8 minutes — CMEs travel at a more leisurely pace,
relatively speaking. At their highest speeds of almost 1,900
miles per second (3,000 kilometers per second), CMEs can
reach Earth in about 15 to 18 hours whilst slower CMEs
traveling around 155 mi/s (250 km/s) can take several days to
arrive, according to the Space Weather Prediction Center of
the National Oceanic and Atmospheric Administration
(NOAA).
9. Impact of CMEs
CMEs can bypass Earth’s magnetic field, unlike the
calmer solar wind.
The aftermath of a CME can screw with electronics
and cause power systems to fail.
Large CMEs can cause technological malfunctions
on Earth and in space: radio transmissions, surges
in electrical currents which overload power grids
causing widespread blackouts, GPS systems,
satellite damage.
10. The Carrington Event
When - 1859
What - besides telegraphs failed, the aurora
borealis lit up the sky due to CMEs bombarded the
Earth.
If a similar storm hits Earth today the technological
systems we depend on would be in complete
disorder. It would cost an estimated 2.6 trillion
dollars.
11. History of Solar Wind Discovery
In 1957 Eugene N. Parker, an astrophysicist theorized
the existence of solar wind.
Eugene Parker described that particles were being
emitted from the sun’s surface. He did the math and
figured out that if the sun’s atmosphere was 1 million
degrees, then particles would come off out of the
corona.
Then, a NASA spacecraft called Mariner II took
readings on it’s journey to Venus, confirming his theory.
12. Solar Wind Chemical Composition
The composition of the solar wind is:
● the ionized hydrogen (electrons and
protons) with an 8% component of helium
● and trace amounts of heavy ions and
atomic nuclei: C, N, O, Ne, Mg, Si, S, and
Fe ripped apart by heating of the Sun's
outer atmosphere, that is, the corona.
SOHO research also identified traces of some
elements for the first time such as P, Ti, Cr
and Ni and an assortment of solar wind
isotopes identified for the first time: Fe 54 and
56; Ni 58,60,62.
13. The Heliophysics System Observatory (HSO) contains a fleet of spacecraft designed to study our dynamic solar system.
The missions study the sun and its influence on the solar system, including the effects of solar wind.
The HSO consists of several solar, heliospheric, geospace and planetary spacecraft including the:
● Parker Solar Probe on a daring mission to "touch" the sun
● Solar and Heliospheric Observatory (SOHO) — a joint effort between NASA and the European Space Agency (ESA)
● Solar Terrestrial Relations Observatory (STEREO) consisting of two near-identical observatories one located ahead
of Earth's orbit and the other trailing behind and ESA's Solar Orbiter that is taking a first time look at the sun's uncharted
polar regions.
14. According to NASA the mission
is "to understand everything
from how planetary
atmospheres have formed, to
how space weather can affect
astronauts and technology near
Earth to the physics that
defines our neighborhood in
space."
The ways and tools to continue
NASA study are on NASA
picture.
15. The Future
In about five billion years, the Sun’s core will run out of hydrogen, the fuel of its fusion reactor. The Sun will continue
to fuse hydrogen in an expanding shell, and this will puff the Sun up into a red giant.
Astrophysicists classify the Sun as a star of average size, temperature and brightness. Due to the very high temperatures found within the Sun, these elements exist not in the gaseous state but as plasma.
The Sun’s corona is the outermost part of the Sun’s atmosphere. The corona is usually hidden by the bright light of the Sun's surface. That makes it difficult to see without using special instruments. However, the corona can be viewed during a total solar eclipse.
The vast amounts of energy emitted by the Sun come from thermonuclear fusion reactions occurring within the core that convert hydrogen nuclei into helium nuclei. It has been calculated that the energy output of the Sun is 3.86 x 1023 kJ per second.
Temperatures within sun`s corona are extremely high, giving some of the charged particles present sufficient energy to escape from the strong gravitational pull of the Sun. This stream of charged particles emanating from the Sun in all directions at speeds of about 400 km/s is called the solar wind. It is rapidly moving plasma that pushes out to the edge of the solar system
Each day, we consciously experience atmospheric weather, driven by radiation from the Sun. The sun’s surface is hot, but the sun’s atmosphere is hotter.
A solar flare is a sudden, explosive release of high-energy particles and radiation from the solar atmosphere. It increases the volume of X-rays and UV light reaching Earth.
The term “space weather” refers to the variable conditions on the sun and in space that can influence the performance of technology we use on Earth.
Here we see the Space Weather Impact. The X-rays can interfere with high-frequency radio communications, and the UV can result in heating of the upper atmosphere, causing it to expand further out into space. Satellites in low-Earth orbit now experience increased drag due to a denser concentration of plasma particles. This alters the orbit of the satellite.
If appropriate alterations to the orbital path cannot be made, the lifetime of the satellite could be substantially reduced.
Space weather can produce electromagnetic fields that induce extreme currents in wires, disrupting power lines, and even causing widespread power outages. Severe space weather also produces solar energetic particles, which can damage satellites used for commercial communications, global positioning, intelligence gathering and weather forecasting.
Solar wind is the movement of charged particles across solar system. The particles’ velocities are highest over coronal holes, areas near the Sun’s poles associated with “open” magnetic field lines that allow material to flow more easily into space. Particles flow out more slowly near the Sun’s equator, where magnetic field lines loop back on themselves and trap coronal material.
Depending on the activity within the Sun’s outer regions, the density and speed of this solar wind can vary from 5–100 protons per cubic centimetre (p/cm3) with speeds between 200–800 km/s. On a typically average day, the speed of the solar wind is about 400 km/s and its density about 10 p/cm3.
Countries with investment in satellite technologies, monitor space weather through a number of agencies such as NOAA, NWS Space Weather Prediction Centre, NASA and European Space Agency. Several New Zealand internet sites take real-time feeds from these agencies.
The Earth’s atmosphere and magnetic field play crucial roles in subduing the damaging effects of both the electromagnetic radiation and solar wind that continually stream out from the Sun.
Our magnetosphere plays the role of gatekeeper, repelling this unwanted energy that’s harmful to life on Earth, trapping most of it a safe distance from Earth’s surface in twin doughnut-shaped zones called the Van Allen Belts.
What in the interaction of the Solar wind and Magnetic Field?
A coronal mass ejection (CME) can release huge amounts of matter and electromagnetic radiation into space above the Sun’s surface. The ejected material is plasma consisting mainly of electrons and protons moving at speeds in the region of 600 km/s. When this interacts with the Earth’s magnetic field, it can cause magnetic field fluctuations that generate rogue electric currents in power transmission lines, submarine communication cables and cross-country pipelines. If large enough, these electric currents can have damaging effects.
CMEs can cause surges in electrical currents which overload power grids causing widespread blackouts. According to NASA, CMEs can jostle Earth's magnetic field which can impair radio transmissions and increase radio static in Earth's ionosphere.
GPS systems are particularly vulnerable to disturbances in the ionosphere and GPS coordinates have been known to stray by tens of feet during a CME event.
The Carrington Event happened in 1859 when massive CME hit Earth - there were even reports of operators receiving electric shocks and sparks showering from telegraph machines, setting papers ablaze.
Interesting, that In 1989, a CME accompanied a solar flare that hit Earth, plunging the entire province of Quebec, Canada, into an electrical blackout that lasted 12-hours, according to a NASA statement. The event cost Quebec's utility company Hydro-Quebec at least $10 million in damages.
Here are a few photos to help feed your imagination if similar storm happens today - cities would look like under the brilliant colors of the Northern Lights.
The solar wind is a collection of streams of energetic particles that originate on the Sun. Ulysses spacecraft measurements show that the solar wind has a "fast" component and a "slow" component. The slow wind has a speed of about 400 km/sec and the fast component is about twice that speed.
Note that although the solar wind is electrically balanced, the solar wind consists almost exclusively of charged particles (stripped away nuclei from atoms) and is an excellent electrical conductor. These electrically conducting particles is technically known as a plasma, so it may be misleading to think of the solar wind as like Earth "winds".
Who study the sun, the solar wind and its impact on the Earth? The HSO!
You can see here the life cycle of the sun – now it has not reached a half. But for now lets enjoy sun and life here on Earth!
Its all for today! I utilized in this presentation research papers from Stanford, Harvard, NASA and other agencies – the list of sources on the next page.
I am happy to entertain any questions !
