STUDENT’SNAME: 1)SARUMATHIA/PR.MUNIANDY 2)MAHALETCHIMIA/PBALAGURU STUDENT’SIC: 1)080627-08-0984 2)080221-08-0570 FORM: 3DAISY(2023) TEACHERNAME:PN.RAHAYUBINTIAMATTOSIRIM THEME: EARTHANDSPACEEXPLORATION LEARNINGAREA: SPACEWEATHER CONTENTSTANDARD: 9.1 THESUN&9.2SPACEWEATHER LEARNINGSTANDARD: 1)9.1.1Explainthe structureofthe sunandphenomena thatoccur theSun’s surface. 2)9.1.2 Justifythe importanceoftheEarthMagnetosphere 3)9.2.1 communicate about spaceweather andits effectsonEarth SCIENCE FORM 3 CHAPTER 9 SPACE WEATHER
ACKNOWLEDGEMENT WE ARE VERY THANKFUL TO OUR SCIENCE TEACHER MDM.RAHAYU BINTI AMAT TOSIRIM AND SCHOOL ADMINISTRATIVE ASSISTANT FOR GIVING US THIS WONDERFUL OPPORTUNITY.OUR SPECIAL THANKS TO DEAREST FRIEND’S AND PARENTS TO GIVES US GOOD IDEAS AND MORE INFORMATION REGARDING THIS PROJECT. HENCE, ALSO MAKE THIS PROJECT COMPLETE IN THE TIME GIVEN. HERE, WE’RE ALSO THANKING TO THE GOD FOR THIS LIFETIME OPPORTUNITY.
NUM CONTENT PAGE 1. My Profile (Our Profile) 1 2. Acknowledgement 2 3. Table of Content 3 4. 9.1 Activities of the Sun that Affect the Earth 4-9 5. 9.2 Space Weather 10-11 6. Our Profile (Chapter 10) 12 7. 10.1 Development in Astronomy 13 8. 10.2 Development of Technology and its Application in Space Exploration 14-16 9. Reference 17 Table of Content
The Sun is the closest ball of hot gas/starto Earth and is at the center of the Solar System The sun is the main source of energy for life on the Earth's surface 9.1 Activities of the Sun that Affect the Earth
The structure of the Sun Corona Radiation Zone Convection Zone Photosphere Chromosph ere Core The structure of the Sun
Core -The innermost part of Earth is the core and is about 1500 miles (2414 km) thick. Both the inner and outer cores consist primarily of iron and nickel. They're extremely hot, with temperatures ranging from 7200–9000℉ (4000–5000℃). Radiation Zone -The radiation zone is the site where energy transport occurs. This zone can be characterized as the place where we, the photons, bounce around, facilitating the ability for energy to be transported to the outer surface of the Sun. The temperature at the radiation zone ranges from 2 to 7 million degrees Celsius. Convection zone -The convection zone is the outer-most layer of the interior. It extends from a depth of 200,000 km up to the visible surface of the Sun. Energy is transported by convection in this region. The surface of the convection zone is where light (photons) is created. Photosphere - The photosphere is a thinner, cooler layer than its neighboring layers. It is only about 500 km (300 miles) wide, a much thinner layer than the interior solar regions. The temperature of the photosphere is around 5,500 °C (9,900 °F), which is much cooler than the Sun's core. Convection zone - The convection zone is the outer-most layer of the interior. It extends from a depth of 200,000 km up to the visible surface of the Sun. Energy is transported by convection in this region. The surface of the convection zone is where light (photons) is created. Chromosphere - The layer on top of the photosphere- The temperature is about 4,400-25,000 ° C with a thickness of about 2,000 km- The chromosphere appears as a red circle around the Moon during a solar eclipse- The red color is produced by hydrogen gas at high temperatures Corona - outermost region of the Sun's atmosphere, consisting of plasma (hot ionized gas). It has a temperature of approximately two million kelvins and an extremely low density. The corona continually varies in size and shape as it is affected by the Sun's magnetic field. CHARACTERISTICS OF THE STRUCTURE OF THE SUN
Solar Winds created by the outward expansion of plasma (a collection of charged particles) from the Sun's corona (outermost atmosphere). This plasma is continually heated to the point that the Sun's gravity can't hold it down. It then travels along the Sun's magnetic field lines that extend radially outward. Granule Each granule is about 1000 km across and is caused by the convection of gas. Hot gas rises in the middle of a granule, and this area appears brighter, then the gas cools and sinks on the edges of the granule and these areas are darker. Granules only last several minutes. Solar Cycle Solar cycles including their maxima and minima, cycle periods and amplitudes, cycle shape, and the nature of active latitudes, hemispheres, and longitudes Solar Flare A solar flare is an intense burst of radiation coming from the release of magnetic energy associated with sunspots. Flares are our solar system's largest explosive events. They are seen as bright areas on the sun and they can last from minutes to hours. Sunspot Sunspots appear as dark spots on the surface of the Sun. Temperatures in the dark centers of sunspots drop to about 3700 K (compared to 5700 K for the surrounding photosphere). They typically last for several days, although very large ones may live for several weeks. Prominences Prominence (also known as a filament when viewed against the solar disk) is a large, bright feature extending outward from the Sun’s surface. Prominences are anchored to the Sun’s surface in the photosphere, and extend outwards into the Sun’s hot outer atmosphere, called the corona The phenomenon that occurs on the surface of the Sun Coronal Mass Ejections large expulsions of plasma and magnetic field from the Sun's corona. They can eject billions of tons of coronal material and carry an embedded magnetic field (frozen in flux) that is stronger than the background solar wind interplanetary magnetic field (IMF) strength.
DEFINITION OF EARTH’S MAGNETOSPHERE a region in outer space surrounding Earth a combination of Earth’s magnetic field (as the prime magnetic field) What is the difference between Earth magnetic field and Earth magnetosphere? The magnetosphere is the region of space surrounding Earth where the dominant magnetic field is the magnetic field of Earth, rather than the magnetic field of interplanetary space Formation of Earth’s Magnetosphere Magnetosphere is formed by the interaction between the magnetic field brought by the solar wind and Earth’s magnetic field. As the number and energy of particles brought by the solar wind change, the shape of the magnetosphere also changes. Earth’ s Magnetosphere and its Importance Shape of Earth’s Magnetosphere (a) Earth’s magnetic field (b) Earth’s magnetosphere
The magnetosphere: • functions as a biological shield to protect life on Earth from the adverse effects of solar wind • blocks charged particles such as electrons, protons and alpha particles in the solar wind from reaching Earth. Excessive numbers of charged particles in Earth’s atmosphere will disrupt telecommunication, navigation system and electric power lines • reduces the pressure exerted by solar wind on Earth’s atmosphere Importance of Earth’s Magnetosphere The importance of magnetosphere is to protect Earth from the adverse effects caused by dangerous particles from the Sun or other bodies in the Universe.
Space weather refers to the environmental conditions in the magnetosphere, ionosphere, and thermosphere as a result of activity occurring on the surface of the Sun (influenced by the solar wind) Solar Radiation Storm Geomagnetic Storm Interpretation of Data on Space Weather Data on space weather is used or analysed to: • forecast when coronal mass ejections occur in the Sun • determine the reasons for the occurrence of solar flares and coronal mass ejections on the surface of the Sun 9.2 Space Weather
Telecommunication interference - The ionosphere is the layer of the atmosphere that serves to reflect radio waves in communication- Geomagnetic storms are temporary disturbances of the Earth’s magnetosphere caused by solar winds or strong radiation eruptions- Electrically charged particles from the Sun enter the ionosphere near the Earth's magnetic poles and ionize the molecules to form electrons and positive ions- This increase in the number of electrons causes the ionosphere to absorb radio waves in the polar regions of the Earth and causes radio interference- These electrically charged particles also interfere with cell phone waves, communication satellites, and aviation radio communication interference Navigation system interference - Interference in the ionosphere can also reduce the accuracy of navigation systems (GPS) used by ships, aircraft and land vehicles- Due to the varying electron densities in the ionosphere as a result of geomagnetic storms- Affects media and telecommunications satellites and can also suffer damage if exposed to radiation Grid power line interference - Geomagnetic storms can cause high electrical currents in long conductors such as power lines (electrical cables). Excessive current will melt the transformer causing damage to the power line system and causing power outage- The strongest solar flare in history was recorded in 1859, the Carrington Event of 1859- The Carrington incident of 1859 damaged the telegraph system in use at the time Aurora Aurora is a colorful light at night in the north pole and south pole.When the Sun is active, many charged particles are released and trapped in the Earth’s magnetic field.Charged particles are carried by the Earth's magnetic field to the north and south poles and collisions occur and interact with nitrogen and oxygen in the upper atmosphere .This interaction produces green, blue, and red lights.The aurora in the northern hemisphere is called the aurora borealis.The aurora in the southern hemisphere is called the aurora australis
STUDENT’S NAME: 1) SARUMATHI A/P R. MUNIANDY 2) MAHALETCHIMI A/P BALAGURU STUDENT’S IC: 1) 080627-08-0984 2) 080221-08-0570 FORM: 3 DAISY (2023) TEACHER NAME: PN.RAHAYU BINTI AMAT TOSIRIM THEME: EARTH AND SPACE EXPLORATION LEARNING AREA: SPACE EXPLORATION CONTENT STANDARD: 10.1 DEVELOPMENT IN ASTRONOMY 10.2 DEVELOPMENT OF TECHNOLOGY AND THEIR APPLICATION IN SPACE EXPLORATION LEARNING STANDARD: 10.1.1 Explain the historical development of the solar system model. 10.2.1 Communicate about the importance of the development of the technology and its application in space exploration. 10.2.2 Justify the need to continue space exploration. SCIENCE FORM 3 CHAPTER 10 SPACE EXPLORATION
Ptolemy Greek astrologer, astronomer and geographer Built the geocentric model with Earth at centre and circular orbit ‘Geo’ means Earth. ‘Centric’ means centre Earth is at the centre of the Solar System Earth is stationary and all the objects such as Sun and planets revolve around its circular orbit Copernicus Polish astronomer, Mathematician, economist and Doctor Built the heliocentric model with the Sun at the centre and circular orbits ‘Helio’ means the Sun ‘Centric’ means centre The Sun is at the centre of the Solar System Earth rotates on its axis and revolves around the Sun in a circular orbit. Kepler German mathematician,astrolog erand astronomer Modified the heliocentric model with the Sun at the common focal point on the elleptical orbit of the planet’s according to the Kepler’s Law 10.1 Development in Astronomy Historical Development of the Solar System Model
1969: First human to set foot on the Moon Neil Armstrong, US Apollo 11 1609: First telescope used in the field of astronoy by Galeleo Galelie 1961: First human to orbit Earth Yuri Gagarin, aboard USSR Vostok 1 1957: First satellite USSR Sputnik 1 1973: First Jupiter flyby – US Pioneer 10 1981: First flight of US space shuttle– Columbia 1989: First Neptune flyby – US Voyager 2 1990: US launched Hubble Space Telescope from space shuttle Discovery 1996: Malaysian satellites MEASAT 1 and 2 launched 2000: Malaysia’s first microsatellite TiungSAT 1 launched 2002: National Space Agency (Agensi Angkasa Negara) established 2011: Construction of International Space Station (ISS) completed 10.2 Development of Technology and its Application in Space Exploration Development in Space Exploration 11th century: Chinese invented gunpowder and used primitive rockets in battles
The astronomical sextant is used to measure the altitude of stars Galileo’s Telescope became the most widely used astronomical instrument Hubble space telescope was placed in an orbit 500 km from the surface of Earth The Spitzer space telescope detects very distant activities in space. Apart from optical telescopes, radiotelescopes are also used to detect radio waves from space. RoRckoectket Rockets are used widely in space explorations. When the fuel in a rocket burns, hot gases are released at high speed through the bottom of the rocket. The release of these gases produces a force which pushes the rocket upwards. Applications of Technology in Space Exploration and their Importance Space Telescope
Satellite The first satellite, Sputnik 1 was sent to outer space in 1957. Space Probe A space probe is a spacecraft that gathers information and sends it back to Earth. Space probes do not orbit Earth like satellites but travel further into and out of the Solar System. Space probes carry cameras and remote sensing instruments as well as radio transmitters and receivers for the purpose of communicating with scientists on Earth. Remote Sensing Remote sensing is a method of gathering and recording information from a distance. In Malaysia, remote sensing instruments are fitted to TiungSAT-1 to receive or detect visible, ultraviolet and infrared lights produced by objects on the surface or below the surface of Earth. The information gathered by TiungSAT-1 is then sent to two data receiving stations at the National Planetarium Station, Federal Territory of Kuala Lumpur and the Mission Control Station (MCGS), Bangi, Selangor. Remote sensing technology is used in various fields in daily life as follows: • Agriculture – To detect suitable regions for agricultural development • Geology – To detect locations such as mineral sources, mass depletion and land depletion • Disaster management – To identify pollution and forest fires • Defence – To detect intrusions of enemy ships, aircraft and vehicles satellite GOES-16 Space probe Cassini
Reference https://science.nasa.gov › resource › the-solar-wind-acr https://ui.adsabs.harvard.edu › abs https://pandai.org Wikipedia https://www.wikipedia.org
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