FRACTAL PHYSICS THEORY - NEUTRINOS AND STARS

Size: px
Start display at page:

Download "FRACTAL PHYSICS THEORY - NEUTRINOS AND STARS"

Transcription

1 Fundamental J. Modern Physics, Vol., Issue 1, 11, Pages 73- Published online at FRACTAL PHYSICS THEORY - NEUTRINOS AND STARS BASF Dispersions and Resins Monaca, Pennsylvania USA Abstract This fifth and last article of the series applies Fractal Physics Theory to neutrinos and stars. A wealth of data has been amassed and significant theoretical progress has been made during the past 4 years centered on detecting and understanding solar neutrinos. The fractal nuclear antineutrino emission process is modeled after quantum scale stellar emission. The absorption and emission of antineutrino energy by stable nuclei and atomic electrons is discussed. Stable nuclei and atomic electrons are at lower lilliputian scale temperatures than decaying nuclei emitting antineutrino energy, consequently, stable matter absorbs relatively high subquantum scale frequency photons and emits relatively low subquantum scale frequency photons in increased numbers so that the total antineutrino energy remains constant. 1. Introduction The first four articles of the Fractal Physics Theory series provide essential background information [1-4]. Fractal Physics Theory (FPT) proposes that most stars are cosmic scale nuclei undergoing cosmic scale beta decay. This cosmic scale nuclear beta decay is argued to occur exactly as nuclear beta decay occurs, the appearance of which differs because of the direction humans look up to larger scales or down to smaller scales of the Fractal Universe. Neutrinos and antineutrinos both arise during quantum scale nuclear fusion and as such are considered to be similar. The totality of a star s radiated energy (electromagnetic Keywords and phrases: fractal physics, neutrinos, starlight, subquantum. Received April 4, Fundamental Research and Development International

2 74 radiation plus neutrinos) over its nuclear burning lifetime comprises one cosmic scale antineutrino. The vast majority of electromagnetic radiations are part of cosmic scale antineutrinos. Familiar antineutrino energy is observed by the lilliputian scale (ls) as electromagnetic radiation and neutrinos. The Sun s energy that constantly bathes the Earth is part of a single cosmic scale antineutrino. It is not so much a matter of seeing an antineutrino as to see with fractal antineutrino energy. Likewise, an antineutrino is the result of an ever spreading sphere of subquantum scale (sqs) photons, which are not in phase, and include a wide range of sqs-frequencies. Antineutrinos in FPT continuously delocalize as they propagate; this differs markedly from antineutrinos described by Modern Physics. A typical star like the Sun is expected to shine in its current state for about 9 billion years (Figure 1), which the titanic scale (ts) measures as 75 ns [1]. A fractally self-similar qs-sun radiates for 75 ns relative to the human scale and y relative to the lilliputian scale. An antineutrino moving at the speed of light for 75 ns travels 5 m in the human scale. This nuclear radiated antineutrino is a spherical pulse 5 m in thickness and composed of a great multitude of sqs-photons and sqs-neutrinos. The spherical shell expanding in matter encounters atoms. The nuclei and electrons of the atoms encountered systematically alter the antineutrino energy. Figure 1. Cosmic scale antineutrino emission (typical shining star).. Antineutrino Quantum Scale Absorption The sqs-photons of relatively high sqs-frequencies comprising the single antineutrino are absorbed by the exposed surfaces of the nuclei and the electrons they encounter. These qs-black bodies reradiate all absorbed sqs-photons spherically from their surfaces, at longer sqs-wavelengths and increased sqs-photon numbers. This spherically radiated cooled sqs-radiation has a net effect, over relatively short

3 FRACTAL PHYSICS THEORY - NEUTRINOS AND STARS 75 distances, of redirecting about half the number of sqs-photons absorbed from the antineutrino expanding shell s initial path. The energy of the antineutrino is initially and continually reduced as it travels short distances ( < 1 cm) through matter. This is similar to Beer s law in analytical chemistry which relates the absorption of electromagnetic radiation traveling through a dilute solution to properties of the solution. However, antineutrino energy is not expected to be reduced when traveling through relatively large volumes of matter. The net effect of continued absorption and emission of antineutrino energy by large volumes of stable matter enables all the transformed antineutrino energy (sqs-photons of lowered sqs-frequencies and increased numbers) to escape the matter. Antineutrino absorption: A ν = abc, (1) A = absorption of antineutrino energy by matter, ν a = atomic surface area exposed to incoming antineutrino energy, b = radial path length traveled by antineutrino energy through matter over short distances, c = atomic number density, d* 1 * N A ( MW ), 3 d = matter density ( kg m ), N = Avogadro s number ( ), A MW = molecular weight. Atomic nuclei and electrons are considered as spheres with surface area 4π R. The expanding neutrino energy shell impinges upon half of the sphere s surface area it encounters. Atomic surface area exposed, a = (# of atomic electrons)(.5)(electron surface area) + (.5)(nuclear surface area). 1 3 a = ( Z ) ( πre ) + π( 1.fm A ), () Z = atomic number of the neutral atom, A = atomic mass, 17 R e = electron s radius ( m ). 3

4 76 Example 1. Uranium 35 dioxide ( 17 ) a U35 = 9* π m + π[( m ) ( ) 1 3 ] 3 = m m = m = b, ( 17 ) a O16 = * π m + π[( m ) ( ) 1 3 ] 31 9 = m m = m =.577 b, a UO = b + *.577 b = 4.63 b, Density 3 = 197 kg m [5], MW = When the initial antineutrino energy is completely absorbed, A ν = 1., and the path length b, can be calculated. b = 1 ( a c ) = 1 [( m ) ( UO UO 7 g m 3 * N )] =.73 m. A single nucleus emitting an antineutrino during beta decay within a solid mass of Uranium 35 dioxide will have its initial antineutrino energy completely absorbed by ambient atomic surfaces within a sphere of radius A.73 cm centered on the decaying nucleus. The nuclear and electron surfaces that absorb the initial antineutrino energy as relatively high sqs-frequency photons immediately reradiate this antineutrino energy as relatively low sqs-frequency photons in increased numbers. A beta decaying process lasting energy at a constant rate. At the end of shell 75 ns continuously emits antineutrino 75 ns, the antineutrino will be a spherical 5 m constant thickness increasing in size at the speed of light. As long as the decaying nucleus is within a large and dense enough mass, the resultant ever expanding antineutrino shell will be composed of the relatively lower sqs-frequency photons.

5 FRACTAL PHYSICS THEORY - NEUTRINOS AND STARS Antineutrino Quantum Scale Emission The totality of all photons emitted from a star s surface comprises about 9% of the energy of a single cosmic scale antineutrino. The remaining % of energy is emitted from the star as neutrinos. Stellar surface temperatures range from < 35 K to > 5 K. These temperatures are converted to their self-similar lilliputian scale stellar surface temperatures using the temperature scaling fractal [1]: T 14 = = [ star, surface temperature] 1, [ star, surface temperature] 1, Nuclei in the process of beta decay have surface ls-temperatures, relative to the human scale, in the range 17 1 < K to > K, which is also the lstemperature range of antineutrinos. It has also been proposed that the surfaces of stable cosmic scale nuclei and atomic electrons are in thermodynamic equilibrium with the microwave background radiation of temperature =.75 K []. The self similar subquantum scale microwave background radiation has a ls-temperature 14 = K, which is the ls-temperature of the vacuum of atoms. Fractal Stephen-Boltzmann equation: 4 m, n m, n m, n m, n [ P( r) ] = [ σ] ε[ A] [ T ], (3) [ P ( r) ], = scaled power radiated, [ σ] m, = scaled Stephen-Boltzmann constant, n ε = emissivity ( < ε < 1), ε = 1 for black bodies, [ A ], = scaled surface area = 4πR, [ T ], = scaled surface temperature, m = object scale location, n = observer scale location. Example. Power radiated by a qs-star fractally self-similar to the Sun 4, 3, 1,, 7 [ P ( r) ] = [ σ] ε[ A] [ T ] = W, (4)

6 7 4 4 [ σ] 3, = ( Wm K ) ( σ = ) ε = 1, = Wm K, 3 [ R ] = ( m) ( Length = ) fm, 1, = 9 [ A ] = m, 1, [ T ] = ( 57 K) ( T = ) =.64 1 K., This beta decaying neutron radiates its antineutrino at the rate of 75 ns W for Example 3. Power radiated and absorbed by a stable 4, 3, 1,, 35 U nucleus [ P ( r) ] = [ σ] ε[ A] [ T ] = W, 49 4 [ σ ] = Wm K, ε = 1, 3, 1 3 1, = [ R ] = 1. fm( ) fm, [ A ] = m, 1, [ T ] = (.75 K) ( T = ) = K., Example 4. Power radiated and absorbed by a ground state atomic electron 4, 3, 1,, 4 [ P ( r) ] = [ σ] ε[ A] [ T ] = W, 49 4 [ σ ] = Wm K, 3, ε = 1, 17 [ R ] = m, 1, 3 [ A ] = m, 1, [ T ] = (.75 K) ( T = ) = K.,

7 FRACTAL PHYSICS THEORY - NEUTRINOS AND STARS 79 Stable nuclei and atomic electrons constantly exchange antineutrino energy with the vacuum. The self-similar local cosmic microwave background radiation is essentially the Sun s reflection off of many ambient liquid Helium mirrors. 4. Solar Neutrinos - Brief Background Luminosity constraint - a sum of the product of solar neutrino fluxes and the energies released by their respective fusion reactions must equal the solar constant, if light element nuclear fusion powers the Sun [6]. ΣΦ a i = [ 4π( 1AU ) ]. (5) i L Table 1 lists the important solar fusion reactions producing the significant portion of electron neutrinos. Included are the average neutrino energies and the amount of reaction energies produced per reaction. Table 1. Solar neutrino flux [6] Flux ( Φ i ) a Reaction E ν ( MeV) a ( MeV) b Φ ( pp) Φ ( pep) Φ ( hep) + p + p H + e + ν e p + e + p H + ν e He + p He + e + ν e Φ ( Be) Be + e Li + νe.14 c Φ ( B) B Be + e + ν e Φ ( N ) N C + e + ν e Φ ( O) O N + e + ν e a Recognized since Hans Bethe s work on fusion reactions that power the sun. i b a i - amount of energy provided to the star by the nuclear fusion reactions associated with the solar neutrino fluxes, Φ i. c 9.7% at.631 MeV and 1.3% at.355 MeV. Table lists important solar neutrino fluxes at the Earth predicted from seven solar models.

8 Table. Predicted solar neutrino fluxes from seven solar models [7] Model pp pep hep 7 Be B 13 N 15 O 17 F BP4(Yale) BP4(Garching) BS BS5 ( N ) BS5(OP) BS5(AGS, OP) BS5(AGS, OPAL) s ( cm ) Table 3 calculates the average neutrino power radiating from the Sun using the average neutrino energies from Table 1 and the BP4(Yale) Solar Model neutrino fluxes from Table. Flux ( Φ i ) Φ i at 1AU ( pp) Table 3. Average neutrino power radiated from the Sun ( cm s 1 ) a Φ ( pep) Φ ( hep) Φ Φ ( Be) Φ ( B) 13 Φ ( N ) 15 Φ ( O) # of ν e second b leaving the Sun a From Table, BP4(Yale) solar model E ( MeV) c Average ν e power ν radiated from Sun ( J s) d Average solar neutrino luminosity, ΣL ν = b From (Table 3, column ) * 4π( cm ) c From Table 1, column 3 d From (Table 3, column 3)*(Table 3, column 4) W

9 FRACTAL PHYSICS THEORY - NEUTRINOS AND STARS 1 The right side of the luminosity constraint, equation (5), is the solar constant. Solar constant L [ 4π( 1AU ) ] = W m, 6 = L = W, solar luminosity [5], 11 1AU = m, 1 astronomical unit is the average earth - sun distance [5]. The left side of the luminosity constraint, equation (5), is calculated in Table 4. Table 4. Luminosity constraint summation Flux Φ i a i ( MeV) a ( Φ at 1 AU m s 1 ) b i aiφ i ( W m ) c Φ ( pp) Φ ( pep) Φ ( hep ) Φ ( Be) Φ ( B) Φ ( N ) Φ ( O ) a From Table 1, column 4 b From Table, BP4(Yale) solar model c From (Table 4, column )*(Table 4, column 3) Σa iφi = It is concluded that the luminosity constraint is met because the solar constant compares with the sum in Table 4. Therefore, the fusion reactions, neutrino fluxes, and neutrino energies listed in the above Tables are accurate representations of solar energy production. Table 5 lists the cs-antineutrino solar lifetime energy.

10 Table 5. Solar cosmic scale antineutrino energy over y Solar Radiation Power (W) Energy (J) % Energy Photons Neutrinos Total The titanic scale identifies this total solar energy radiated as single antineutrino..57 MeV of a In Fractal Physics Theory, an antineutrino located in the cosmic scale is measured by the human scale as mostly quantum scale electromagnetic radiation and a few percent quantum scale neutrinos: [ antineutrino, composition] 1, = ~ 9% [ photons] 1, + ~ % [ neutrinos] 1, The ~ % neutrinos can be further subdivided into mostly subquantum scale photons and a few percent sqs-neutrinos: % [ neutrinos] 1, = ~ 1.96% [ photons] + ~.4% [ neutrinos] 3, ~ 3, This process of subdividing the neutrinos into lower scales of photons and neutrinos continues indefinitely. 5. Solar Neutrino Transformation The Sun s photon luminosity over emission of a single neutrino y is scaled down to approximate the Fractal Wien s displacement law: [ λ ] [ T ] = [ b], (6) m m, n m, n m, n [ λ m ] m, n = scaled wavelength of maximum intensity, [ T ] m, n = scaled surface temperature, [ b ] m, n = scaled Wien s constant, 3 [ b], = mk [5],

11 FRACTAL PHYSICS THEORY - NEUTRINOS AND STARS 3 m = object scale location, n = observer scale location. Example 5. Subquantum scale self-similar to the Sun λ m of sqs-photons radiated by a qs-star fractally 3 [ λ ] = [ b] [ T ] = m, m 3,,, [ b ] = ( mk ) ( Wie = ) = mk,, [ T ] = 57 K ( T = ) =.64 1 K., Fractal photon frequency-wavelength relation: [ λ ] [ f ], (7) m, n m, n = c [ λ ] m, n = scaled photon wavelength, [ f ] m, n = scaled photon frequency, c = m s, m = object scale location, n = observer scale location. Example 6. Sqs-frequency of sqs-photons radiated by a qs-star fractally selfsimilar to the Sun Fractal photon energy relation: 3 3 [ f ] = c ( m ) =.66 1 Hz. 3, [ E ], = scaled photon energy, [ h ], = scaled Planck s constant, [ h] = , [ E ] = [ h] [ f ], () 34 m, n m, n m, n Js, [ h ] = ( Js) ( h = ) = Js, 3,

12 4 [ f ], = scaled photon frequency, m = object scale location, n = observer scale location. Example 7. Human scale observed energy of sqs-photons radiated by a qs-star fractally self-similar to the Sun 3 [ photon, E] [ ] (.66 1 Hz ) 3, = h 3, = Joules =. 1 ev. Individual subquantum scale photon energies comprising the bulk of a neutrino are infinitesimal! Example. Approximate # of sqs-photons composing 1 neutrino emitted by a qs-star fractally self-similar to the Sun From Example 7 14 neutrino energy = (power = W ) ( 75 ns) = J, # of sqs-photons = ( J ) ( J ) = Example 9. Let all the sqs-photons of the neutrino of Example be absorbed and reemitted by stable atomic surfaces. Stable atomic surfaces radiate sqs-photons with the following properties: [ T ] = (.75K ) ( T = ) = K,, 7 [ ] =.6 1 m, λ m 3, 35 [ f ] = Hz, m 3, [ photon, E ] = J = 9. 1 ev. 3, Example 1. Approximate # of sqs-photons composing the reemitted neutrino energy # of sqs-photons = ( J ) ( J ) = Fractal Physics Theory proposes that solar neutrinos do not oscillate but have 6 65

13 FRACTAL PHYSICS THEORY - NEUTRINOS AND STARS 5 their energies transformed by interactions with stable atomic surfaces that reduce the 79 initial individual sqs-photon energies to J, and increase the # of initial sqs-photons by a factor proportional to 14 [ fusing nuclei, surface temperature ] [ K ]., 6. Neutrino Subquantum Scale Electromagnetic Radiation Spectrum The Sun emits electromagnetic radiation approximately as Planck s radiation law; therefore the majority component of neutrino energy is modeled with a lilliputian scale (ls) version of Planck s radiation law. Fractal Planck's radiation law: 5 x 1 [ I ( λ, T )] = A[ λ] ( e 1), (9) m, n [ I ( λ, T )] = scaled intensity radiated per unit λ at a given T, A = πc [ h], m, n x = [ h] c ([ λ] [ k] [ T ] ), m, n m, n m, n m, n [ h ], = scaled Planck constant, [ λ] m, = scaled wavelength, n [ k ], = scaled Boltzmann constant, [ T ], = scaled temperature, m = object scale location, n = observer scale location. 5 x 1 [ I ( λ, T )] = A[ λ] ( e 1), (1), 3, [ I ( λ, T )], = ls-intensity radiated per unit λ at a given T, A = πc [ h], 3, x = [ h] c ([ λ] [ k] [ T ] ), 3, 3, 3,, 114 [ h ] = Js, 3,

14 6 [ λ ] 3, = sqs-wavelength, 94 [ k ] = J K, 3, [ T ], = ls-temperature, c = m s, e =.711. Equation 1 is used to generate data in Tables 6 and 7 at the lilliputian scale temperatures self-similar to.75 K and 57 K. Figures and 3 plot the data from Tables 6 and 7, respectively, for sqs-wavelengths versus intensity radiated per sqswavelength. At first glance the power densities listed in Tables 6 and 7 may appear startling high. However, this just reflects the minute scales of sqs-wavelengths, nuclear surface areas, and emission times involved. Consider: ( W m )( m )( m )( s ) =.4 MeV, is reasonable for neutrinos. 9 Table 6. Neutrino lilliputian scale radiation [.75 K] = K 7, [ ] λ 3, ( 1 7 m ) [ ] 5 5 3, ( m x A λ ) ( e 1) 1 [ 3 I ( λ, T )], ( W m )

15 FRACTAL PHYSICS THEORY - NEUTRINOS AND STARS 7 Figure. Single neutrino lilliputian scale radiation spectrum from Table 6 data; Neutrino lilliputian scale radiation [ T.75 K] = K. =, Table 7. Neutrino lilliputain scale radiation [ 57 K] = K 14, [ ] λ 1, ( 1 3 m ) [ ] 5 5 A λ 1, ( m ) x ( e 1) 1 [ I ( λ, T )] 1, ( W 3 m )

16 Figure 3. Single neutrino lilliputian scale radiation spectrum from Table 7 data; Neutrino quantum scale radiation [ T 57 K] =.64 1 K. =, Conclusion This fifth article of the series applies Fractal Physics Theory to neutrinos and stars. Several human scale radiation equations are generalized to scale, while the lilliputian scale radiation equations are used to model neutrino emission. The subquantum scale electromagnetic radiation portion of solar core produced neutrinos should arrive at the Earth similar to the plots in Figure. References [1] L. J. Malinowski, Fractal Physics Theory - Foundation, Fundamental J. Modern Physics 1() (11), [] L. J. Malinowski, Fractal Physics Theory - Cosmic Scale Nuclear Explosion Cosmology, Fundamental J. Modern Physics 1() (11), [3] L. J. Malinowski, Fractal Physics Theory - Electrons, Photons, Wave-Particles, and Atomic Capacitors, Fundamental J. Modern Physics 1() (11), [4] L. J. Malinowski, Fractal Physics Theory - Nucleons and the Strong Force, Fundamental J. Modern Physics (1) (11), 3-7. [5] D. R. Lide, editor, Handbook of Chemistry and Physics, CRC Press, Boca Raton, FL, 6. [6] John N. Bahcall, The luminosity constraint on solar neutrino fluxes, Physical Review C, Volume 65, 51. [7] John N. Bahcall et al., New solar opacities, abundances, helioseismology, and neutrino fluxes, Astrophys. J. 61 (5), L5-L.

Stellar Structure. Observationally, we can determine: Can we explain all these observations?

Stellar Structure. Observationally, we can determine: Can we explain all these observations? Stellar Structure Observationally, we can determine: Flux Mass Distance Luminosity Temperature Radius Spectral Type Composition Can we explain all these observations? Stellar Structure Plan: Use our general

More information

Class XII Chapter 13 - Nuclei Physics

Class XII Chapter 13 - Nuclei Physics Question 13.1: (a) Two stable isotopes of lithium and have respective abundances of 7.5% and 92.5%. These isotopes have masses 6.01512 u and 7.01600 u, respectively. Find the atomic mass of lithium. (b)

More information

Question 13.1: Two stable isotopes of lithium and have respective abundances of 7.5% and 92.5%. These isotopes have masses 6.01512 u and 7.01600 u, respectively. Find the atomic mass of lithium. Boron

More information

10/4/2011. Tells you the number of protons

10/4/2011. Tells you the number of protons Atomic Structure The arrangement of the subatomic particles within the atom determines the chemical properties of the elements How they interact with one another The types of ions and structures that they

More information

Properties of Light and Atomic Structure. Chapter 7. So Where are the Electrons? Electronic Structure of Atoms. The Wave Nature of Light!

Properties of Light and Atomic Structure. Chapter 7. So Where are the Electrons? Electronic Structure of Atoms. The Wave Nature of Light! Properties of Light and Atomic Structure Chapter 7 So Where are the Electrons? We know where the protons and neutrons are Nuclear structure of atoms (Chapter 2) The interaction of light and matter helps

More information

Today. Homework Due. Stars. Properties (Recap) Nuclear Reactions. proton-proton chain. CNO cycle. Stellar Lifetimes

Today. Homework Due. Stars. Properties (Recap) Nuclear Reactions. proton-proton chain. CNO cycle. Stellar Lifetimes Today Stars Properties (Recap) Nuclear Reactions proton-proton chain CNO cycle Stellar Lifetimes Homework Due Stellar Properties Luminosity Surface Temperature Size Mass Composition Stellar Properties

More information

Take away concepts. What is Energy? Solar Radiation Emission and Absorption. Energy: The ability to do work

Take away concepts. What is Energy? Solar Radiation Emission and Absorption. Energy: The ability to do work Solar Radiation Emission and Absorption Take away concepts 1. 2. 3. 4. 5. 6. Conservation of energy. Black body radiation principle Emission wavelength and temperature (Wien s Law). Radiation vs. distance

More information

Properties of Electromagnetic Radiation Chapter 5. What is light? What is a wave? Radiation carries information

Properties of Electromagnetic Radiation Chapter 5. What is light? What is a wave? Radiation carries information Concepts: Properties of Electromagnetic Radiation Chapter 5 Electromagnetic waves Types of spectra Temperature Blackbody radiation Dual nature of radiation Atomic structure Interaction of light and matter

More information

Sources of radiation

Sources of radiation Sources of radiation Most important type of radiation is blackbody radiation. This is radiation that is in thermal equilibrium with matter at some temperature T. Lab source of blackbody radiation: hot

More information

1 Light from all distant galaxies is found to be shifted towards longer wavelengths. The more distant the galaxy, the greater the shift in wavelength.

1 Light from all distant galaxies is found to be shifted towards longer wavelengths. The more distant the galaxy, the greater the shift in wavelength. 1 Light from all distant galaxies is found to be shifted towards longer wavelengths. The more distant the galaxy, the greater the shift in wavelength. State the conclusions that we can draw from this.

More information

The Sun. Nearest Star Contains most of the mass of the solar system Source of heat and illumination

The Sun. Nearest Star Contains most of the mass of the solar system Source of heat and illumination The Sun Nearest Star Contains most of the mass of the solar system Source of heat and illumination Outline Properties Structure Solar Cycle Energetics Equation of Stellar Structure TBC Properties of Sun

More information

Introduction and Fundamental Observations

Introduction and Fundamental Observations Notes for Cosmology course, fall 2005 Introduction and Fundamental Observations Prelude Cosmology is the study of the universe taken as a whole ruthless simplification necessary (e.g. homogeneity)! Cosmology

More information

LIGHT. Question. Until very recently, the study of ALL astronomical objects, outside of the Solar System, has been with telescopes observing light.

LIGHT. Question. Until very recently, the study of ALL astronomical objects, outside of the Solar System, has been with telescopes observing light. LIGHT Question Until very recently, the study of ALL astronomical objects, outside of the Solar System, has been with telescopes observing light. What kind of information can we get from light? 1 Light

More information

Introduction to the Sun

Introduction to the Sun Lecture 15 Introduction to the Sun Jiong Qiu, MSU Physics Department Open Q: what physics do we learn about the Sun? 1. Energy - nuclear energy - magnetic energy 2. Radiation - continuum and line emissions;

More information

Astronomy 182: Origin and Evolution of the Universe

Astronomy 182: Origin and Evolution of the Universe Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 11 Nov. 13, 2015 Today Cosmic Microwave Background Big Bang Nucleosynthesis Assignments This week: read Hawley and Holcomb,

More information

ASTR-1010: Astronomy I Course Notes Section IV

ASTR-1010: Astronomy I Course Notes Section IV ASTR-1010: Astronomy I Course Notes Section IV Dr. Donald G. Luttermoser Department of Physics and Astronomy East Tennessee State University Edition 2.0 Abstract These class notes are designed for use

More information

Chemistry (

Chemistry ( Question 2.1: (i) Calculate the number of electrons which will together weigh one gram. (ii) Calculate the mass and charge of one mole of electrons. Answer 2.1: (i) Mass of one electron = 9.10939 10 31

More information

Light and Atoms

Light and Atoms Light and Atoms ASTR 170 2010 S1 Daniel Zucker E7A 317 zucker@science.mq.edu.au ASTR170 Introductory Astronomy: II. Light and Atoms 1 Overview We ve looked at telescopes, spectrographs and spectra now

More information

1. Star: A object made of gas found in outer space that radiates.

1. Star: A object made of gas found in outer space that radiates. 1. Star: A object made of gas found in outer space that radiates. 2. Stars produce extremely great quantities of energy through the process of. The chemical formula for nuclear fusion looks like this:

More information

11/19/08. Gravitational equilibrium: The outward push of pressure balances the inward pull of gravity. Weight of upper layers compresses lower layers

11/19/08. Gravitational equilibrium: The outward push of pressure balances the inward pull of gravity. Weight of upper layers compresses lower layers Gravitational equilibrium: The outward push of pressure balances the inward pull of gravity Weight of upper layers compresses lower layers Gravitational equilibrium: Energy provided by fusion maintains

More information

Nuclear Physics and Nuclear Reactions

Nuclear Physics and Nuclear Reactions Slide 1 / 33 Nuclear Physics and Nuclear Reactions The Nucleus Slide 2 / 33 Proton: The charge on a proton is +1.6x10-19 C. The mass of a proton is 1.6726x10-27 kg. Neutron: The neutron is neutral. The

More information

[2] State in what form the energy is released in such a reaction.... [1]

[2] State in what form the energy is released in such a reaction.... [1] (a) The following nuclear reaction occurs when a slow-moving neutron is absorbed by an isotope of uranium-35. 0n + 35 9 U 4 56 Ba + 9 36Kr + 3 0 n Explain how this reaction is able to produce energy....

More information

Physics 126 Practice Exam #4 Professor Siegel

Physics 126 Practice Exam #4 Professor Siegel Physics 126 Practice Exam #4 Professor Siegel Name: Lab Day: 1. Light is usually thought of as wave-like in nature and electrons as particle-like. In which one of the following instances does light behave

More information

Problem Set 2 Solutions

Problem Set 2 Solutions Problem Set 2 Solutions Problem 1: A A hot blackbody will emit more photons per unit time per unit surface area than a cold blackbody. It does not, however, necessarily need to have a higher luminosity,

More information

QUANTUM NEWTONIAN GRAVITY WORKING MODEL

QUANTUM NEWTONIAN GRAVITY WORKING MODEL QUANTUM NEWTONIAN GRAVITY WORKING MODEL (Gravitation by Radiation) Leonard J. Malinowski LJMalinowski@gmail.com MARCH 21, 2019 PUBLISHED BY SCALATIVITY LLC Scalativity.com Abstract A quantum theory of

More information

Today. Spectra. Thermal Radiation. Wien s Law. Stefan-Boltzmann Law. Kirchoff s Laws. Emission and Absorption. Spectra & Composition

Today. Spectra. Thermal Radiation. Wien s Law. Stefan-Boltzmann Law. Kirchoff s Laws. Emission and Absorption. Spectra & Composition Today Spectra Thermal Radiation Wien s Law Stefan-Boltzmann Law Kirchoff s Laws Emission and Absorption Spectra & Composition Spectrum Originally, the range of colors obtained by passing sunlight through

More information

23 Astrophysics 23.5 Ionization of the Interstellar Gas near a Star

23 Astrophysics 23.5 Ionization of the Interstellar Gas near a Star 23 Astrophysics 23.5 Ionization of the Interstellar Gas near a Star (8 units) No knowledge of Astrophysics is assumed or required: all relevant equations are defined and explained in the project itself.

More information

aka Light Properties of Light are simultaneously

aka Light Properties of Light are simultaneously Today Interaction of Light with Matter Thermal Radiation Kirchhoff s Laws aka Light Properties of Light are simultaneously wave-like AND particle-like Sometimes it behaves like ripples on a pond (waves).

More information

James Maxwell ( )

James Maxwell ( ) From Atoms To Stars James Maxwell (1831 1879) Finalized the work of others on electricity and magnetism. He formulated Maxwell Equations for the electromagnetic field. His equations predicted the existence

More information

INTRODUCTION Radiation differs from conduction and convection in that it does not require the presence of a material medium to take place.

INTRODUCTION Radiation differs from conduction and convection in that it does not require the presence of a material medium to take place. RADIATION INTRODUCTION Radiation differs from conduction and convection in that it does not require the presence of a material medium to take place. Radiation: The energy emitted by matter in the form

More information

The Sun. The Sun is a star: a shining ball of gas powered by nuclear fusion. Mass of Sun = 2 x g = 330,000 M Earth = 1 M Sun

The Sun. The Sun is a star: a shining ball of gas powered by nuclear fusion. Mass of Sun = 2 x g = 330,000 M Earth = 1 M Sun The Sun The Sun is a star: a shining ball of gas powered by nuclear fusion. Mass of Sun = 2 x 10 33 g = 330,000 M Earth = 1 M Sun Radius of Sun = 7 x 10 5 km = 109 R Earth = 1 R Sun Luminosity of Sun =

More information

Chapter 6. Atoms and Starlight

Chapter 6. Atoms and Starlight Chapter 6 Atoms and Starlight What is light? Light is an electromagnetic wave. Wavelength and Frequency wavelength frequency = speed of light = constant Particles of Light Particles of light are called

More information

1. The most important aspects of the quantum theory.

1. The most important aspects of the quantum theory. Lecture 5. Radiation and energy. Objectives: 1. The most important aspects of the quantum theory: atom, subatomic particles, atomic number, mass number, atomic mass, isotopes, simplified atomic diagrams,

More information

Primordial (Big Bang) Nucleosynthesis

Primordial (Big Bang) Nucleosynthesis Primordial (Big Bang) Nucleosynthesis H Li Be Which elements? He METALS - 1942: Gamow suggests a Big Bang origin of the elements. - 1948: Alpher, Bethe & Gamow: all elements are synthesized minutes after

More information

The Nature of Light I: Electromagnetic Waves Spectra Kirchoff s Laws Temperature Blackbody radiation

The Nature of Light I: Electromagnetic Waves Spectra Kirchoff s Laws Temperature Blackbody radiation The Nature of Light I: Electromagnetic Waves Spectra Kirchoff s Laws Temperature Blackbody radiation Electromagnetic Radiation (How we get most of our information about the cosmos) Examples of electromagnetic

More information

ZX or X-A where X is chemical symbol of element. common unit: [unified mass unit = u] also known as [atomic mass unit = amu] or [Dalton = Da]

ZX or X-A where X is chemical symbol of element. common unit: [unified mass unit = u] also known as [atomic mass unit = amu] or [Dalton = Da] 1 Part 5: Nuclear Physics 5.1. The Nucleus = atomic number = number of protons N = neutron number = number of neutrons = mass number = + N Representations: X or X- where X is chemical symbol of element

More information

Astronomy 1102 Exam #1 Chapters 1,2,5,6 & 16

Astronomy 1102 Exam #1 Chapters 1,2,5,6 & 16 Astronomy 1102 Exam #1 Chapters 1,2,5,6 & 16 Chapter 1 Degrees- basic unit of angle measurement, designated by the symbol -a full circle is divided into 360 and a right angle measures 90. arc minutes-one-sixtieth

More information

The Amazing Power of Starlight

The Amazing Power of Starlight The Amazing Power of Starlight Chapter 6 Just by analyzing the light received from a star, astronomers can retrieve information about a star s Starlight and Atoms 1. Total energy output 2. Surface temperature

More information

Interactions. Laws. Evolution

Interactions. Laws. Evolution Lecture Origin of the Elements MODEL: Origin of the Elements or Nucleosynthesis Fundamental Particles quarks, gluons, leptons, photons, neutrinos + Basic Forces gravity, electromagnetic, nuclear Interactions

More information

From Last Time: We can more generally write the number densities of H, He and metals.

From Last Time: We can more generally write the number densities of H, He and metals. From Last Time: We can more generally write the number densities of H, He and metals. n H = Xρ m H,n He = Y ρ 4m H, n A = Z Aρ Am H, How many particles results from the complete ionization of hydrogen?

More information

Astr 1050 Mon. March 30, 2015 This week s Topics

Astr 1050 Mon. March 30, 2015 This week s Topics Astr 1050 Mon. March 30, 2015 This week s Topics Chapter 14: The Sun, Our Star Structure of the Sun Physical Properties & Stability Photosphere Opacity Spectral Line Formation Temperature Profile The Chromosphere

More information

Visit for more fantastic resources. Edexcel. A Level. A Level Physics. Astrophysics 1 (Answers) Name: Total Marks: /30

Visit   for more fantastic resources. Edexcel. A Level. A Level Physics. Astrophysics 1 (Answers) Name: Total Marks: /30 Visit http://www.mathsmadeeasy.co.uk/ for more fantastic resources. Edexcel A Level A Level Physics Astrophysics 1 (Answers) Name: Total Marks: /30 Maths Made Easy Complete Tuition Ltd 2017 1. Amongst

More information

Ay 1 Lecture 8. Stellar Structure and the Sun

Ay 1 Lecture 8. Stellar Structure and the Sun Ay 1 Lecture 8 Stellar Structure and the Sun 8.1 Stellar Structure Basics How Stars Work Hydrostatic Equilibrium: gas and radiation pressure balance the gravity Thermal Equilibrium: Energy generated =

More information

Physics Important Terms and their Definitions

Physics Important Terms and their Definitions Physics Important Terms and their S.No Word Meaning 1 Acceleration The rate of change of velocity of an object with respect to time 2 Angular Momentum A measure of the momentum of a body in rotational

More information

NUCLEI. Atomic mass unit

NUCLEI. Atomic mass unit 13 NUCLEI Atomic mass unit It is a unit used to express the mass of atoms and particles inside it. One atomic mass unit is the mass of atom. 1u = 1.660539 10. Chadwick discovered neutron. The sum of number

More information

Stellar Astrophysics: The Continuous Spectrum of Light

Stellar Astrophysics: The Continuous Spectrum of Light Stellar Astrophysics: The Continuous Spectrum of Light Distance Measurement of Stars Distance Sun - Earth 1.496 x 10 11 m 1 AU 1.581 x 10-5 ly Light year 9.461 x 10 15 m 6.324 x 10 4 AU 1 ly Parsec (1

More information

Lasers PH 645/ OSE 645/ EE 613 Summer 2010 Section 1: T/Th 2:45-4:45 PM Engineering Building 240

Lasers PH 645/ OSE 645/ EE 613 Summer 2010 Section 1: T/Th 2:45-4:45 PM Engineering Building 240 Lasers PH 645/ OSE 645/ EE 613 Summer 2010 Section 1: T/Th 2:45-4:45 PM Engineering Building 240 John D. Williams, Ph.D. Department of Electrical and Computer Engineering 406 Optics Building - UAHuntsville,

More information

Neutron-to-proton ratio

Neutron-to-proton ratio Neutron-to-proton ratio After one second, the Universe had cooled to 10 13 K. The Universe was filled with protons, neutrons, electrons, and neutrinos. The temperature was high enough that they interconverted

More information

THE NUCLEUS: A CHEMIST S VIEW Chapter 20

THE NUCLEUS: A CHEMIST S VIEW Chapter 20 THE NUCLEUS: A CHEMIST S VIEW Chapter 20 "For a long time I have considered even the craziest ideas about [the] atom[ic] nucleus... and suddenly discovered the truth." [shell model of the nucleus]. Maria

More information

The physics of stars. A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure.

The physics of stars. A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure. Lecture 4 Stars The physics of stars A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure. X-ray ultraviolet infrared radio To understand

More information

The Sun = Typical Star

The Sun = Typical Star The Sun = Typical Star Some Properties Diameter - 109 times Earth s Volume - about 1,000,000 times Earth s Mass - about 300,000 times Earth s 99.8% of Solar System Density = Mass/Volume = 1.4 g/cm 3 The

More information

ME 476 Solar Energy UNIT TWO THERMAL RADIATION

ME 476 Solar Energy UNIT TWO THERMAL RADIATION ME 476 Solar Energy UNIT TWO THERMAL RADIATION Unit Outline 2 Electromagnetic radiation Thermal radiation Blackbody radiation Radiation emitted from a real surface Irradiance Kirchhoff s Law Diffuse and

More information

LIFE CYCLE OF A STAR

LIFE CYCLE OF A STAR LIFE CYCLE OF A STAR First stage = Protostar PROTOSTAR Cloud of gas and dust many light-years across Gravity tries to pull the materials together Eventually, at the center of the ball of dust and gas,

More information

The Sun. October 21, ) H-R diagram 2) Solar Structure 3) Nuclear Fusion 4) Solar Neutrinos 5) Solar Wind/Sunspots

The Sun. October 21, ) H-R diagram 2) Solar Structure 3) Nuclear Fusion 4) Solar Neutrinos 5) Solar Wind/Sunspots The Sun October 21, 2002 1) H-R diagram 2) Solar Structure 3) Nuclear Fusion 4) Solar Neutrinos 5) Solar Wind/Sunspots Review Blackbody radiation Measuring stars distance luminosity brightness and distance

More information

Quantum Mechanics. Exam 3. Photon(or electron) interference? Photoelectric effect summary. Using Quantum Mechanics. Wavelengths of massive objects

Quantum Mechanics. Exam 3. Photon(or electron) interference? Photoelectric effect summary. Using Quantum Mechanics. Wavelengths of massive objects Exam 3 Hour Exam 3: Wednesday, November 29th In-class, Quantum Physics and Nuclear Physics Twenty multiple-choice questions Will cover:chapters 13, 14, 15 and 16 Lecture material You should bring 1 page

More information

MIDSUMMER EXAMINATIONS 2001 PHYSICS, PHYSICS WITH ASTROPHYSICS PHYSICS WITH SPACE SCIENCE & TECHNOLOGY PHYSICS WITH MEDICAL PHYSICS

MIDSUMMER EXAMINATIONS 2001 PHYSICS, PHYSICS WITH ASTROPHYSICS PHYSICS WITH SPACE SCIENCE & TECHNOLOGY PHYSICS WITH MEDICAL PHYSICS No. of Pages: 6 No. of Questions: 10 MIDSUMMER EXAMINATIONS 2001 Subject PHYSICS, PHYSICS WITH ASTROPHYSICS PHYSICS WITH SPACE SCIENCE & TECHNOLOGY PHYSICS WITH MEDICAL PHYSICS Title of Paper MODULE PA266

More information

Conceptos generales de astrofísica

Conceptos generales de astrofísica Tema 14 Conceptos generales de astrofísica Asignatura de Física Nuclear Curso académico 2009/2010 Universidad de Santiago de Compostela 1 1. Nuclear Astrophysic s domain Nuclear Astrophysics is a relatively

More information

Basic science. Atomic structure. Electrons. The Rutherford-Bohr model of an atom. Electron shells. Types of Electrons. Describing an Atom

Basic science. Atomic structure. Electrons. The Rutherford-Bohr model of an atom. Electron shells. Types of Electrons. Describing an Atom Basic science A knowledge of basic physics is essential to understanding how radiation originates and behaves. This chapter works through what an atom is; what keeps it stable vs. radioactive and unstable;

More information

PhysicsAndMathsTutor.com 1

PhysicsAndMathsTutor.com 1 PhysicsAndMathsTutor.com 1 1. Describe briefly one scattering experiment to investigate the size of the nucleus of the atom. Include a description of the properties of the incident radiation which makes

More information

1 Stellar Energy Generation Physics background

1 Stellar Energy Generation Physics background 1 Stellar Energy Generation Physics background 1.1 Relevant relativity synopsis We start with a review of some basic relations from special relativity. The mechanical energy E of a particle of rest mass

More information

The Stars. Chapter 14

The Stars. Chapter 14 The Stars Chapter 14 Great Idea: The Sun and other stars use nuclear fusion reactions to convert mass into energy. Eventually, when a star s nuclear fuel is depleted, the star must burn out. Chapter Outline

More information

Visit for more fantastic resources. OCR. A Level. A Level Physics. Astrophysics 1 (Answers) Name: Total Marks: /30

Visit   for more fantastic resources. OCR. A Level. A Level Physics. Astrophysics 1 (Answers) Name: Total Marks: /30 Visit http://www.mathsmadeeasy.co.uk/ for more fantastic resources. OCR A Level A Level Physics Astrophysics 1 (Answers) Name: Total Marks: /30 Maths Made Easy Complete Tuition Ltd 2017 1. Amongst all

More information

Week 8: Stellar winds So far, we have been discussing stars as though they have constant masses throughout their lifetimes. On the other hand, toward

Week 8: Stellar winds So far, we have been discussing stars as though they have constant masses throughout their lifetimes. On the other hand, toward Week 8: Stellar winds So far, we have been discussing stars as though they have constant masses throughout their lifetimes. On the other hand, toward the end of the discussion of what happens for post-main

More information

Examination Radiation Physics - 8N120 5 November 2014, 13:30-16:30

Examination Radiation Physics - 8N120 5 November 2014, 13:30-16:30 Examination Radiation Physics - 8N120 5 November 2014, 13:30-16:30 Four general remarks: This exam consists of 8 assignments on a total of 3 pages. There is a table on page 4 listing the maximum number

More information

IB Physics - Astronomy

IB Physics - Astronomy Solar System Our Solar System has eight planets. The picture below shows their relative sizes, but NOT their relative distances. A planet orbits the sun, and has gravitationally cleared its orbital area

More information

Stellar Nucleosynthesis

Stellar Nucleosynthesis Stellar Nucleosynthesis What makes the sun shine? Gravita7onal contrac7on Chemical reac7ons Nucleosynthesis Stellar Nucleosynthesis The PP chain The CNO cycle The Triple alpha process and on to Fe Stellar

More information

Physics 6C. Final Practice Solutions. Prepared by Vince Zaccone For Campus Learning Assistance Services at UCSB

Physics 6C. Final Practice Solutions. Prepared by Vince Zaccone For Campus Learning Assistance Services at UCSB Physics 6C Final Practice Solutions Use the following information for problems 1 and. A beam of white light with frequency between 4.00 x 10 14 Hz and 7.90 x 10 14 Hz is incident on a sodium surface, which

More information

Nicholas J. Giordano. Chapter 30. Nuclear Physics. Marilyn Akins, PhD Broome Community College

Nicholas J. Giordano.   Chapter 30. Nuclear Physics. Marilyn Akins, PhD Broome Community College Nicholas J. Giordano www.cengage.com/physics/giordano Chapter 30 Nuclear Physics Marilyn Akins, PhD Broome Community College Atomic Nuclei Rutherford s discovery of the atomic nucleus caused scientists

More information

Physics 3204 UNIT 3 Test Matter Energy Interface

Physics 3204 UNIT 3 Test Matter Energy Interface Physics 3204 UNIT 3 Test Matter Energy Interface 2005 2006 Time: 60 minutes Total Value: 33 Marks Formulae and Constants v = f λ E = hf h f = E k + W 0 E = m c 2 p = h λ 1 A= A T 0 2 t 1 2 E k = ½ mv 2

More information

Introduction to Nuclear Reactor Physics

Introduction to Nuclear Reactor Physics Introduction to Nuclear Reactor Physics J. Frýbort, L. Heraltová Department of Nuclear Reactors 19 th October 2017 J. Frýbort, L. Heraltová (CTU in Prague) Introduction to Nuclear Reactor Physics 19 th

More information

Our sole source of light and heat in the solar system. A very common star: a glowing g ball of gas held together by its own gravity and powered

Our sole source of light and heat in the solar system. A very common star: a glowing g ball of gas held together by its own gravity and powered The Sun Visible Image of the Sun Our sole source of light and heat in the solar system A very common star: a glowing g ball of gas held together by its own gravity and powered by nuclear fusion at its

More information

Physics 6C. Final Practice Solutions. Prepared by Vince Zaccone For Campus Learning Assistance Services at UCSB

Physics 6C. Final Practice Solutions. Prepared by Vince Zaccone For Campus Learning Assistance Services at UCSB Physics 6C Final Practice Solutions Use the following information for problems 1 and. A beam of white light with frequency between 4.00 x 10 14 Hz and 7.90 x 10 14 Hz is incident on a sodium surface, which

More information

3/26/2018. Atoms Light and Spectra. Topics For Today s Class. Reminder. Topics For Today s Class. The Atom. Phys1403 Stars and Galaxies

3/26/2018. Atoms Light and Spectra. Topics For Today s Class. Reminder. Topics For Today s Class. The Atom. Phys1403 Stars and Galaxies Foundations of Astronomy 13e Seeds Foundations of Astronomy 13e Seeds Phys1403 Stars and Galaxies Instructor: Dr. Goderya Chapter 7 Atoms Light and Spectra Reminder Homework for Chapter 5, 6 and 7 is posted

More information

Astronomy 242: Review Questions #3 Distributed: April 29, 2016

Astronomy 242: Review Questions #3 Distributed: April 29, 2016 Astronomy 242: Review Questions #3 Distributed: April 29, 2016 Review the questions below, and be prepared to discuss them in class next week. Modified versions of some of these questions will be used

More information

COX & GIULI'S PRINCIPLES OF STELLAR STRUCTURE

COX & GIULI'S PRINCIPLES OF STELLAR STRUCTURE COX & GIULI'S PRINCIPLES OF STELLAR STRUCTURE Extended Second Edition A. Weiss, W. Hillebrandt, H.-C. Thomas and H. Ritter Max-Planck-lnstitut fur Astrophysik, Garching, Germany C S P CONTENTS PREFACE

More information

ASTRONOMY 1 EXAM 3 a Name

ASTRONOMY 1 EXAM 3 a Name ASTRONOMY 1 EXAM 3 a Name Identify Terms - Matching (20 @ 1 point each = 20 pts.) Multiple Choice (25 @ 2 points each = 50 pts.) Essays (choose 3 of 4 @ 10 points each = 30 pt 1.Luminosity D 8.White dwarf

More information

The Sun. How are these quantities measured? Properties of the Sun. Chapter 14

The Sun. How are these quantities measured? Properties of the Sun. Chapter 14 The Sun Chapter 14 The Role of the Sun in the Solar System > 99.9% of the mass Its mass is responsible for the orderly orbits of the planets Its heat is responsible for warming the planets It is the source

More information

Announcements. - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11

Announcements. - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11 Announcements - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11 Review for Test #2 Oct 11 Topics: The Solar System and its Formation The Earth and our Moon

More information

Nucleosynthesis. W. F. McDonough 1. Neutrino Science, Tohoku University, Sendai , Japan. (Dated: Tuesday 24 th April, 2018)

Nucleosynthesis. W. F. McDonough 1. Neutrino Science, Tohoku University, Sendai , Japan. (Dated: Tuesday 24 th April, 2018) Nucleosynthesis W. F. McDonough 1 1 Department of Earth Sciences and Research Center for Neutrino Science, Tohoku University, Sendai 980-8578, Japan (Dated: Tuesday 24 th April, 2018) Goals Where were

More information

Examination Radiation Physics - 8N120, 2 November

Examination Radiation Physics - 8N120, 2 November Examination Radiation Physics - 8N0, November 0-4.00-7.00 Four general remarks: This exam consists of 6 assignments on a total of pages. There is a table on page listing the maximum number of that can

More information

LIFE CYCLE OF A STAR

LIFE CYCLE OF A STAR LIFE CYCLE OF A STAR First stage = Protostar PROTOSTAR Cloud of gas and dust many light-years across Gravity tries to pull the materials together Eventually, at the center of the ball of dust and gas,

More information

is the minimum stopping potential for which the current between the plates reduces to zero.

is the minimum stopping potential for which the current between the plates reduces to zero. Module 1 :Quantum Mechanics Chapter 2 : Introduction to Quantum ideas Introduction to Quantum ideas We will now consider some experiments and their implications, which introduce us to quantum ideas. The

More information

CHEMISTRY Topic #1: Atomic Structure and Nuclear Chemistry Fall 2017 Dr. Susan Findlay See Exercises 2.3 to 2.6

CHEMISTRY Topic #1: Atomic Structure and Nuclear Chemistry Fall 2017 Dr. Susan Findlay See Exercises 2.3 to 2.6 CHEMISTRY 1000 Topic #1: Atomic Structure and Nuclear Chemistry Fall 2017 Dr. Susan Findlay See Exercises 2.3 to 2.6 Balancing Nuclear Reactions mass number (A) atomic number (Z) 12 6 C In an ordinary

More information

Stars and their properties: (Chapters 11 and 12)

Stars and their properties: (Chapters 11 and 12) Stars and their properties: (Chapters 11 and 12) To classify stars we determine the following properties for stars: 1. Distance : Needed to determine how much energy stars produce and radiate away by using

More information

Title Gravitational lensing and the proton-proton reaction

Title Gravitational lensing and the proton-proton reaction Title Gravitational lensing and the proton-proton reaction Author Rodney Bartlett Abstract This article is a longer and more complete version of a comment I posted on Nature journal s website. Go to the

More information

Stellar Composition. How do we determine what a star is made of?

Stellar Composition. How do we determine what a star is made of? Stars Essential Questions What are stars? What is the apparent visual magnitude of a star? How do we locate stars? How are star classified? How has the telescope changed our understanding of stars? What

More information

The Sun Closest star to Earth - only star that we can see details on surface - easily studied Assumption: The Sun is a typical star

The Sun Closest star to Earth - only star that we can see details on surface - easily studied Assumption: The Sun is a typical star The Sun Closest star to Earth - only star that we can see details on surface - easily studied Assumption: The Sun is a typical star Why is the Sun hot and bright? Surface Temperature of the Sun: T =

More information

Chapter 9 The Sun. Nuclear fusion: Combining of light nuclei into heavier ones Example: In the Sun is conversion of H into He

Chapter 9 The Sun. Nuclear fusion: Combining of light nuclei into heavier ones Example: In the Sun is conversion of H into He Our sole source of light and heat in the solar system A common star: a glowing ball of plasma held together by its own gravity and powered by nuclear fusion at its center. Nuclear fusion: Combining of

More information

Today The Sun. Events

Today The Sun. Events Today The Sun Events Last class! Homework due now - will count best 5 of 6 Final exam Dec. 20 @ 12:00 noon here Review this Course! www.case.edu/utech/course-evaluations/ The Sun the main show in the solar

More information

chapter 31 Stars and Galaxies

chapter 31 Stars and Galaxies chapter 31 Stars and Galaxies Day 1:Technology and the Big Bang Studying the Stars A. Telescopes - Electromagnetic radiation emitted by stars and other objects include light, radio, and X-ray Space telescopes

More information

Fundamental Stellar Parameters. Radiative Transfer. Stellar Atmospheres. Equations of Stellar Structure

Fundamental Stellar Parameters. Radiative Transfer. Stellar Atmospheres. Equations of Stellar Structure Fundamental Stellar Parameters Radiative Transfer Stellar Atmospheres Equations of Stellar Structure Nuclear Reactions in Stellar Interiors Binding Energy Coulomb Barrier Penetration Hydrogen Burning Reactions

More information

Fundamental Forces. Range Carrier Observed? Strength. Gravity Infinite Graviton No. Weak 10-6 Nuclear W+ W- Z Yes (1983)

Fundamental Forces. Range Carrier Observed? Strength. Gravity Infinite Graviton No. Weak 10-6 Nuclear W+ W- Z Yes (1983) Fundamental Forces Force Relative Strength Range Carrier Observed? Gravity 10-39 Infinite Graviton No Weak 10-6 Nuclear W+ W- Z Yes (1983) Electromagnetic 10-2 Infinite Photon Yes (1923) Strong 1 Nuclear

More information

Matter and Energy. Previous studies have taught us that matter and energy cannot be created nor destroyed We balance equations to obey this law.

Matter and Energy. Previous studies have taught us that matter and energy cannot be created nor destroyed We balance equations to obey this law. Fission & Fusion Matter and Energy Previous studies have taught us that matter and energy cannot be created nor destroyed We balance equations to obey this law. 2 H 2 O 2 H 2 + O 2 We now need to understand

More information

AST 301 Introduction to Astronomy

AST 301 Introduction to Astronomy AST 301 Introduction to Astronomy John Lacy RLM 16.332 471-1469 lacy@astro.as.utexas.edu Myoungwon Jeon RLM 16.216 471-0445 myjeon@astro.as.utexas.edu Bohua Li RLM 16.212 471-8443 bohuali@astro.as.utexas.edu

More information

ASTR Midterm 1 Phil Armitage, Bruce Ferguson

ASTR Midterm 1 Phil Armitage, Bruce Ferguson ASTR 1120-001 Midterm 1 Phil Armitage, Bruce Ferguson FIRST MID-TERM EXAM FEBRUARY 16 th 2006: Closed books and notes, 1 hour. Please PRINT your name and student ID on the places provided on the scan sheet.

More information

Activity 12: Energy from Nuclear Reactions

Activity 12: Energy from Nuclear Reactions Name Section Activity 12: Energy from Nuclear Reactions 12.1 A Model of the Composition of Nucleons 1) Formation of Nucleons Nucleons consist of quark trios. a) Place orange or green quarks into the metal

More information

Barrier Penetration, Radioactivity, and the Scanning Tunneling Microscope

Barrier Penetration, Radioactivity, and the Scanning Tunneling Microscope Physics 5K Lecture Friday April 20, 2012 Barrier Penetration, Radioactivity, and the Scanning Tunneling Microscope Joel Primack Physics Department UCSC Topics to be covered in Physics 5K include the following:

More information

= : K A

= : K A Atoms and Nuclei. State two limitations of JJ Thomson s model of atom. 2. Write the SI unit for activity of a radioactive substance. 3. What observations led JJ Thomson to conclusion that all atoms have

More information

Physics 107: Ideas of Modern Physics

Physics 107: Ideas of Modern Physics Physics 107: Ideas of Modern Physics Exam 3 Nov. 30, 2005 Name ID # Section # On the Scantron sheet, 1) Fill in your name 2) Fill in your student ID # (not your social security #) 3) Fill in your section

More information

MockTime.com. Ans: (b) Q6. Curie is a unit of [1989] (a) energy of gamma-rays (b) half-life (c) radioactivity (d) intensity of gamma-rays Ans: (c)

MockTime.com. Ans: (b) Q6. Curie is a unit of [1989] (a) energy of gamma-rays (b) half-life (c) radioactivity (d) intensity of gamma-rays Ans: (c) Chapter Nuclei Q1. A radioactive sample with a half life of 1 month has the label: Activity = 2 micro curies on 1 8 1991. What would be its activity two months earlier? [1988] 1.0 micro curie 0.5 micro

More information