What is the flux dn(t) generated by solenoid 1's magnetic field through a single turn of solenoid 2? Express ?1(t) in terms of h(t), quantities given in the introduction, and any needed constants. Constants| Periodic Table Learning Goal View Available Hint(s) To learn about mutual inductance from an example of a long solenoid with two windings To illustrate the calculation of mutual inductance it is helpful to consider the specific example of two solenoids that are wound on a common cylinder. We will take the cylinder to have radius p and length L. Assume that the solenoid is much longer than its radius, so that its field can be determined from Ampère's law throughout its entire length: $B(F) dlend i(t)Bi (t)p ous Answe Correct (Figure 1) We will consider the field that arises from solenoid 1 which has n1 turns per unit length. The magnetic field due to solenoid 1 passes (entirely, in this case) through solenoid 2, which has n2 turns per unit length. Any change in magnetic flux from the field generated by solenoid 1 induces an EMF in solenoid 2 through Faraday's law of induction Part C Now find the electromotive force E2 (t) induced across the entirety of solenoid 2 by the change in current in solenoid 1. Remember that both solenoids have en Express your answer in terms of dl, (t)/dt, n, n2, other parameters given in the introduction, and any relevant constants View Available Hint(s) Figure 1 of 1 &2(t) Submit Radius p Part D This question will be shown after you complete previous question(s) Part E This question will be shown after you complete previous question (s) Blue coi n turns per unit length Part F This question will be shown after you complete previous question (s) Black coil: ni turns per unit length Provide Feedback Next >

  sequence  is a continuous and distinctive band of  stars  that appears on plots of stellar  color  versus  brightness. these color-magnitude plots are known as  hertzsprung–russell diagramsafter their co-developers,  ejnar hertzsprungand  henry norris russell. stars on this band are known as  main-sequence stars  or  dwarf stars. these are the most numerous true stars in the universe, and include the earth's  sun.after condensation and ignition of a star, it generates  thermal energy  in its dense core region through  nuclear fusion  of  hydrogen  into  helium. during this stage of the star's lifetime, it is located on the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and age. the cores of main-sequence stars are in  hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of  gravitational collapse  from the overlying layers. the strong dependence of the rate of energy generation on temperature and pressure to sustain this balance. energy generated at the core makes its way to the surface and is radiated away at the  photosphere. the energy is carried by either  radiation  or  convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.the main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. stars below about 1.5 times the  mass of the sun  (1.5  m☉) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the  proton–proton chain. above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of  carbon,  nitrogen  and  oxygen  as intermediaries in the  cno cycle  that produces helium from hydrogen atoms. main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. below this mass, stars have cores that are entirely radiative with convective zones near the surface. with decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases. main-sequence stars below 0.4  m☉undergo convection throughout their mass. when core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.in general, the more massive a star is, the shorter its lifespan on the main sequence. after the hydrogen fuel at the core has been consumed, the star  evolves  away from the main sequence on the hr diagram, into a  supergiant,  red giant, or directly to a  white dwarf.

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One splits the atoms and molecules  the other combines them