Solar Physics and Sun-Earth Connection ( introduction ) Samuel Danagoulian NC A&T State University Teacher’s Workshop, 1-27-05.

Slides:



Advertisements
Similar presentations
The Sun The Sun is a star. The Sun is a star. It is 4,500 million years old It is 4,500 million years old It takes 8 minutes for its light to reach.
Advertisements

The Sun 6.E.1.2 Explain why Earth sustains life while other planets do not based on their properties (including types of surface, atmosphere.
The Sun 6.E.1.2 Explain why Earth sustains life while other planets do not based on their properties (including types of surface, atmosphere.
Our Star, the Sun Chapter Eighteen.
Chapter 9 The Sun.
The Sun.
The Sun – Our Star Chapter 7:. General Properties Average star Absolute visual magnitude = 4.83 (magnitude if it were at a distance of 32.6 light years)
Review Vocabulary magnetic field: the portion of space near a magnetic or current-carrying body where magnetic forces can be detected The Sun contains.
Guiding Questions 1.What is the source of the Sun’s energy? 2.What is the internal structure of the Sun? 3.How can we measure the properties of the Sun’s.
Copyright © 2012 Pearson Education, Inc. Radius: 6.9  10 8 m (109 times Earth) Mass: 2  kg (300,000 Earths) Luminosity: 3.8  watts Our Star.
The Sun Chapter 10.
The Sun Chapter 7:. General Properties Average star Absolute visual magnitude = 4.83 (magnitude if it were at a distance of 32.6 light years) Central.
7 THE SUN The star we see by day. 7 Goals Summarize the overall properties of the Sun. What are the different parts of the Sun? Where does the light we.
The star we see but seldom notice
The Sun The Sun in X-rays over several years The Sun is a star: a shining ball of gas powered by nuclear fusion. Luminosity of Sun = 4 x erg/s =
Astronomy Picture of the Day. The Sun Core temperature - 15 million K Surface temperature K 99.9% of all of the matter in the solar system Entirely.
THE SUN 1 million km wide ball of H, He undergoing nuclear fusion. Contains 99% of the mass in the whole solar system! Would hold 1.3 million earths!
The Sun’s Energy Composition of the Sun
Youtube: Secrets of a Dynamic Sun The Sun – Our Star
The Sun. Sun Considered a medium STAR 93,000,000 miles away from Earth 1.39 million kilometers in diameter (one million Earths can fit inside the sun.
EARTH & SPACE SCIENCE Chapter 29 The Sun 29.2 Solar Activity.
Note key, please leave in binder. Our Sun
THE SUN AND STARS And anything I want to put in here.
The Sun Earth Science - Mr. Gallagher. The Sun is the Earth's nearest star. Similar to most typical stars, it is a large ball of hot electrically charged.
The Sun Our Nearest Star. The Source of the Sun’s Energy The Source of the Sun’s Energy Fusion of light elements into heavier elements. Hydrogen converts.
Lesson 3.3: The Sun.
The Sun Internal structure of the Sun Nuclear fusion –Protons, neutrons, electrons, neutrinos –Fusion reactions –Lifetime of the Sun Transport of energy.
The Sun Section 26.1.
Chapter 9 The Sun. 9.4 The Active Sun Sunspots: appear dark because slightly cooler than surroundings:
Lecture 13. Review: Static Stellar structure equations Hydrostatic equilibrium: Mass conservation: Equation of state: Energy generation: Radiation Convection.
The Sun Unit 5 PESS 2. Energy from the Sun Electromagnetic energy is a type of energy that can travel through space an example is visible light Light.
Our Star, the Sun Chapter Eighteen. The Sun’s energy is generated by thermonuclear reactions in its core The energy released in a nuclear reaction corresponds.
The Sun ROBOTS Summer Solar Structure Core - the center of the Sun where nuclear fusion releases a large amount of heat energy and converts hydrogen.
Solar Energy p-p chain is source of Solar Energy Sun could last 1.
THE SUN The star we see by day.
EARTH SCIENCE Prentice Hall EARTH SCIENCE Tarbuck Lutgens 
Stars Physics Astrophysics. Brightness Different brightness. Different color. How bright are they really? What is due to distance? What is due.
The Sun.
THE SUN. The Sun The sun has a diameter of 900,000 miles (>100 Earths could fit across it) >1 million Earths could fit inside it. The sun is composed.
Lecture 19: The Sun Our Star Some Facts about the Sun  distance from Earth: 1.5 x 10 8 km  luminosity: 3.86 x W  mass: 1.98 x kg (3.33.
Solar Properties Has more than 99% the mass of our solar system Has more than 99% the mass of our solar system Diameter: 1,390,000 km Diameter: 1,390,000.
Chapter 9 Our Star, the Sun. What do you think? What is the surface of the Sun like? Does the Sun rotate? What makes the Sun shine?
The Sun Unit 6: Astronomy.
Structure of the Sun 24.3 The Sun  Because the sun is made of gas, no sharp boundaries exist between its various layers. Keeping this in mind, we can.
1. active prominences - solar prominences that change in a matter of hours.
The Sun – Our Star Our sun is considered an “average” star and is one of the 100 BILLION stars that make up the Milky Way galaxy. But by no MEANS does.
PHYS 1621 Proton-proton cycle 3 steps. PHYS 1622 Layers of the Sun Mostly Hydrogen with about 25% Helium. Small amounts of heavier elements Gas described.
Structure of the Sun 24.3 The Sun  Because the sun is made of gas, no sharp boundaries exist between its various layers.  Keeping this in mind, we can.
Chapter 14 Our Star.
The Sun By: JGilliam The Sun’s CompositionIdentifying Stars Composition ▪ Hydrogen and Helium together make up 99% of the sun’s mass. ▪ 75% of the sun’s.
Our Sun.
Unit 8 Chapter 29 The Sun. We used to think that our sun was a ball of fire in the sky. Looking at our sun unaided will cause blindness. The Sun’s Energy.
Chapter 10 Our Star.
P Spring 2002 L18Richard Kass The Solar Neutrino Problem M&S Since 1968 R.Davis and collaborators have been measuring the cross section of:
Universe Tenth Edition Chapter 16 Our Star, the Sun Roger Freedman Robert Geller William Kaufmann III.
Outer Layers of the Sun Photosphere –Limb darkening –Sun spots Chromosphere Corona Prominences, flares, coronal mass ejections Reading
Chapter 28 The Sun Section 2 Solar Activity Notes 28-2.
Chapter 29. Sec 1 Structure of the sun People believed the sun’s energy came from fire They believed the sun burned some type of fuel to produce energy.
© 2017 Pearson Education, Inc.
The Sun.
The Sun Unit 1B : Astronomy.
The Sun and Our Earth The Structure of Our Sun The Energy of Our Sun
The Sun Unit 6: Astronomy.
The Sun: Our Star.
The Sun.
Section 2: Solar Activity
The Sun and Our Earth The Structure of Our Sun The Energy of Our Sun
The Sun.
The Centre of the Solar System Earth Science 11
The sun gives off tremendous amounts of energy
Presentation transcript:

Solar Physics and Sun-Earth Connection ( introduction ) Samuel Danagoulian NC A&T State University Teacher’s Workshop,

Solar Data  Solar radius = 695,990 km = 432,470 mi = 109 Earth radii  Solar mass = kg = lb = 333,000 Earth masses  Solar luminosity (energy output of the Sun) = erg/s  Surface temperature = 5770 K = 10,400 ºF  Surface density = g/cm 3 = Air density  Surface composition = 70% H, 28% He, 2% (C, N, O,...) by mass

Solar Data (cont.)  Central temperature = 15,600,000 K = 28,000,000 ºF  Central density = 150 g/cm3 = 8 × Gold density  Central composition = 35% H, 63% He, 2% (C, N, O,...) by mass  Solar age = yr  Solar Rotation: period 27 days  Solar Cycles: ~11 years, ~ 22 years

Solar Structure 15x10 6 K 6000 K X-rays and UV, 1x10 6 K Magnetic filed causes formation of Sunspots, flares, mass ejections

Introduction to Nuclear Physics  Molecular force is Electromagnetic: (long range) Atoms are held together by a dipole force which has an origin of Electro-Magnetism Atoms are held together by a dipole force which has an origin of Electro-Magnetism  Atom=nucleus + (orbiting electrons) The force between nucleus and electrons has EM origin  Nucleus= few nucleons together (protons and neutrons) The force between nucleons is STRONG (nuclear) which is present and attractive only at short distances. Between two protons, in addition, there is Electromagnetic force, which is repulsive. In order to create a stable nucleus, one needs to dilute the charged nuclear matter (protons) with neutral particles (neutrons). STRONG force is 137 times stronger than EM force. The force between nucleons is STRONG (nuclear) which is present and attractive only at short distances. Between two protons, in addition, there is Electromagnetic force, which is repulsive. In order to create a stable nucleus, one needs to dilute the charged nuclear matter (protons) with neutral particles (neutrons). STRONG force is 137 times stronger than EM force.

Particle Zoo PARTICLESSIZEMASS (AMU)  Molecules10 -8 m Atoms m1-260 Atoms m1-260 Nucleus < m 1-260Nucleus < m Heavy Particles (BARIONS) Heavy Particles (BARIONS) Nucleons: (p, n), hyperons m1 – 1.5Nucleons: (p, n), hyperons m1 – 1.5 Light Particles (MESONS) < m Light Particles (MESONS) < m regular, strange, charm, top, bottom0.14 – 10regular, strange, charm, top, bottom0.14 – QUARKS (u, d, s, c, t, b) < m QUARKS (u, d, s, c, t, b) < m GAUGE Particles( , W +-, Z 0, g) GAUGE Particles( , W +-, Z 0, g) LEPTONS< m LEPTONS< m Electron, mu, tau (e,  ) Electron, mu, tau (e,  ) Neutrino - electron, mu, tau ( e, ,  )0 (?)Neutrino - electron, mu, tau ( e, ,  )0 (?) GAUGE particles provide interaction between particles and quarks

Nuclear Binding Energy

Solar Energy  Thermonuclear reactions, pp-chain (98% of energy) p+p  d+e + + e (neutrino energy is 0.42 MeV) p+e - + p  d+ e (1.44 MeV) p+d  3 He+  p+d  3 He+  3 He+ 3 He  4 He+2p 3 He+p  4 He+e + + e (18.8 MeV) 3 He+ 4 He  7 Be+  7 Be+e -  7 Li+  (0.38, 0.86 MeV) 7 Be+e -  7 Li+  (0.38, 0.86 MeV) 7 Li+ p  8 Be+  8 Be  2 4 He

Solar Structure 15x10 6 K 6000 K X-rays and UV, 1x10 6 K Magnetic filed causes formation of Sunspots, flares, mass ejections

Modeling of Solar Mechanism  Mechanical and thermal equilibrium Pressure gradient balances gravitational force Pressure gradient balances gravitational force Solar energy radiation is balanced by the thermonuclear energy of the core Solar energy radiation is balanced by the thermonuclear energy of the core  Energy transportation from the core to the surface: to the 1/3 of the radius from the surface, where the opacity is high (Radiative envelope); to the 1/3 of the radius from the surface, where the opacity is high (Radiative envelope); Convective envelope Convective envelope Radiation to the outer space through Photosphere and Chromosphere Radiation to the outer space through Photosphere and Chromosphere  Numerical Integration of the process: the constraints: Observed mass, radius, luminosity and ratio of chemical abundances by mass. Observed mass, radius, luminosity and ratio of chemical abundances by mass.

Solar Neutrino puzzle Chlorine experiment (Davis, ) 615 tons Liquid perchloroethylene (Homestake gold mine in South Dakota ) 37 Cl+  37 Ar+e - (threshold=0.814 MeV) Prediction from Solar Model Calculations: ( ) SNU Experimental result: ( ) SNU Japanese Experiment (Kamioka mine, 1996) 680 tons of water. Super-K: +e -  +e - (threshold=5.5 MeV, e - cherenkov light in the water). Experimental result: low rate, flavour change GALLEX, SAGE, GNO (1999, Gallium experiments) Experimental result: low rate SNO (Sudbury Neutrino Observatory, heavy water experiment) Experimental result: neutrino flavour change

SNO results confirmed Super-K results on e count rate. There are three types of neutrinos: e  and  Neutrino oscillates from one flavour to another during it’s long journey to the Earth. KamLAND experiment (2003, detection of neutrinos from the reactor): confirmed the results of SNO and calculated the parameter responsible for the mixing of flavors.

Solar Flares 

Coronal Loops

 Coronal loops are found around sunspots and in active regions. These structures are associated with the closed magnetic field lines that connect magnetic regions on the solar surface. Many coronal loops last for days or weeks but most change quite rapidly  Some loops, however, are associated with solar flares and are visible for much shorter periods. These loops contain denser material than their surroundings. The three-dimensional structure and the dynamics of these loops is an area of active research. solar flaresthree-dimensional structuresolar flaresthree-dimensional structure

Solar Flares SOHO

Solar Flares (cont)

Solar Flare  is defined as a sudden and intense variation in solar brightness. The solar magnetic energy is suddenly released. Radiation occurs in the entire electromagnetic spectrum, (radio waves to X- and  -rays). The first solar flare recorded in astronomical literature was on September 1, Radiation electromagnetic spectrum  -rays Radiation electromagnetic spectrum  -rays

Polar Plumes SOHO

Polar Plumes  Polar plumes are long thin streamers that project outward from the Sun's north and south poles. These structures are associated with the "open" magnetic field lines at the Sun's poles. The plumes are formed by the action of the solar wind in much the same way as the peaks on the helmet streamers.

Solar Flares, Solar Wind SOHO

Solar Wind

Coronal Holes SOHO

 Coronal holes are regions where the corona is dark. These features were discovered with X-ray telescopes above the earth's atmosphere observing the solar disc. Coronal holes are associated with "open" magnetic field lines and are often found at the Sun's poles. The high-speed solar wind is known to originate in coronal holes. solar wind solar wind

Solar Activity

Solar Activity and Geomagnetic storm

Aurora

Aurora  Is caused by high energy particles (mainly electrons) interacting with the Earth's atmosphere over the North Pole. Due to the interaction of electrons with atoms of the air, an excitation of latter takes place following by the emission of the light quanta which removes the excitation of the atom.

Aurora (cont.)  This process is called scintillation of the air due to the passage of electrons through it. The spectrum of the light emission is in the UV- visible range, depending of the nature of the gas and maximum energy of the particles. The intensity of the emission depends on the intensity of electrons.

Aurora from the space

Aurora (cont.)  The effect of interaction of many electrons with atoms results in the Aurora that can be clearly seen during some nights in the higher latitude close to the North Pole. Since electrons mainly originate from the sun, the intensity depends greatly on the status of the solar activity.

Aurora (cont.)  However, the energy of electrons is not enough high to excite the air atoms unless they are accelerated in the way to the earth's atmosphere. The acceleration occurs during the disturbance of the geomagnetic field of the Earth, during geomagnetic storm.

Aurora (cont.)  The idea is that the geomagnetic field is responding to a disturbance from the Sun due to magnetic explosions on the Sun's corona and coronal mass ejection towards the Earth. The geomagnetic field of the Earth changes due to the flux of magnetic field, releasing energy and thereby accelerating electrons and other particles to high energies.

Aurora (cont.)  These particles are bent in the geomagnetic field to spiral along the magnetic field lines. Some amount of particles end up in the upper part of the earth's atmosphere causing the auroral mechanism to begin jan.curtis

Aurora (cont.)

Happy New Year !