New Application Center Additions
http://www.maplesoft.com/applications
en-us2017 Maplesoft, A Division of Waterloo Maple Inc.Maplesoft Document SystemMon, 23 Oct 2017 00:41:06 GMTMon, 23 Oct 2017 00:41:06 GMTThe latest content added to the Application Centerhttp://www.mapleprimes.com/images/mapleapps.gifNew Application Center Additions
http://www.maplesoft.com/applications
Plot of equation impulse-momentum
https://www.maplesoft.com/applications/view.aspx?SID=154347&ref=Feed
In this application you can visualize the impulse generated by a constant and variable force for the interaction of a particle with an object in a state of rest or movement. It is also the calculation of the momentum-momentum equation by entering the mass of the particle to solve initial and final velocities respectively according to the case study. Engineering students can quickly display the calculations and then their interpretation.<img src="/view.aspx?si=154347/mivis.png" alt="Plot of equation impulse-momentum" align="left"/>In this application you can visualize the impulse generated by a constant and variable force for the interaction of a particle with an object in a state of rest or movement. It is also the calculation of the momentum-momentum equation by entering the mass of the particle to solve initial and final velocities respectively according to the case study. Engineering students can quickly display the calculations and then their interpretation.154347Tue, 17 Oct 2017 04:00:00 ZProf. Lenin Araujo CastilloProf. Lenin Araujo CastilloThe Sounds of Nature
https://www.maplesoft.com/applications/view.aspx?SID=154346&ref=Feed
This application takes various sounds throughout nature and displays them as spectrographs. Examples include crickets, a tornado, thunder, hail, a bee, and a purring cat.<img src="/view.aspx?si=154346/spectograph.JPG" alt="The Sounds of Nature" align="left"/>This application takes various sounds throughout nature and displays them as spectrographs. Examples include crickets, a tornado, thunder, hail, a bee, and a purring cat.154346Thu, 12 Oct 2017 04:00:00 ZDaniel ChesloDaniel ChesloMoment of a force using vectors
https://www.maplesoft.com/applications/view.aspx?SID=154345&ref=Feed
The development of the calculation of moments using force vectors is clearly observed by taking a point and also a line. Different exercises are solved with the help of Maple syntax. We can also visualize the vector behavior in the different configurations of the position vector. Applications designed exclusively for engineering students. In Spanish.<img src="/view.aspx?si=154345/moment of force.PNG" alt="Moment of a force using vectors" align="left"/>The development of the calculation of moments using force vectors is clearly observed by taking a point and also a line. Different exercises are solved with the help of Maple syntax. We can also visualize the vector behavior in the different configurations of the position vector. Applications designed exclusively for engineering students. In Spanish.154345Tue, 26 Sep 2017 04:00:00 ZProf. Lenin Araujo CastilloProf. Lenin Araujo CastilloRadiative Flux
https://www.maplesoft.com/applications/view.aspx?SID=154299&ref=Feed
Calculate the solar constant, the flux density of the Sun through a Johnson B filter, and the flux and temperature of the Sun.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Radiative Flux" align="left"/>Calculate the solar constant, the flux density of the Sun through a Johnson B filter, and the flux and temperature of the Sun.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154299Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryGalaxy fluxes
https://www.maplesoft.com/applications/view.aspx?SID=154300&ref=Feed
Calculate the ratio of the fluxes of the Andromeda galaxy and NGC 5236 (M83).<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Galaxy fluxes" align="left"/>Calculate the ratio of the fluxes of the Andromeda galaxy and NGC 5236 (M83).<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154300Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryPlanck's law, Stefan-Boltzmann law, Wien's law
https://www.maplesoft.com/applications/view.aspx?SID=154301&ref=Feed
Based on Planck's law for radiance, calculate (A) the Stefan-Boltzmann law for flux, (B) Wien's displacement law and (C) the colour index for the following ranges of two colour filters: blue: 400-500 nm; red: 600-700 nm.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Planck's law, Stefan-Boltzmann law, Wien's law" align="left"/>Based on Planck's law for radiance, calculate (A) the Stefan-Boltzmann law for flux, (B) Wien's displacement law and (C) the colour index for the following ranges of two colour filters: blue: 400-500 nm; red: 600-700 nm.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154301Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryLuminosity
https://www.maplesoft.com/applications/view.aspx?SID=154302&ref=Feed
(A) Find the number which, when raised to the fifth power, equals 100. Then derive the formula relating magnitudes to fluxes. (B) Find the absolute magnitude of Sirius and the Sun. (C) Calculate the bolometric magnitude of Antares. Calculate its radius, given the corrected bolometric magnitude. Calculate the temperature of Rigil Kent. (D) Find the bolometric correction of Sirius.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Luminosity" align="left"/>(A) Find the number which, when raised to the fifth power, equals 100. Then derive the formula relating magnitudes to fluxes. (B) Find the absolute magnitude of Sirius and the Sun. (C) Calculate the bolometric magnitude of Antares. Calculate its radius, given the corrected bolometric magnitude. Calculate the temperature of Rigil Kent. (D) Find the bolometric correction of Sirius.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154302Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryRadiative Pressure
https://www.maplesoft.com/applications/view.aspx?SID=154303&ref=Feed
A circular solar sail with 100% reflectivity and a radius (R) of 600 m. is at rest in the Earth's orbit. The sail is oriented so that its normal points directly to the Sun. The total mass of the sail and its payload "(m[sail]" ) is 900 kg. The sail moves toward Mars along a trajectory of increasing r. As it does so, its velocity (v) and acceleration (a) increase. Calculate the radiative pressure on the sail, a(r), v(r), v at the orbit of Mars, and how many days are required to reach Mars <BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Radiative Pressure" align="left"/>A circular solar sail with 100% reflectivity and a radius (R) of 600 m. is at rest in the Earth's orbit. The sail is oriented so that its normal points directly to the Sun. The total mass of the sail and its payload "(m[sail]" ) is 900 kg. The sail moves toward Mars along a trajectory of increasing r. As it does so, its velocity (v) and acceleration (a) increase. Calculate the radiative pressure on the sail, a(r), v(r), v at the orbit of Mars, and how many days are required to reach Mars <BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154303Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberrySynchrotron Radiation: the Crab Nebula
https://www.maplesoft.com/applications/view.aspx?SID=154304&ref=Feed
About 6500 years ago, a star in the constellation of Taurus exploded as a supernova. On July 4, 1054 CE, light from this explosion reached the Earth and was observed by Chinese astronomers, who made a record of their observation. The Crab Nebula has been identified as the detritus from the explosion; and in the approximately 960 years since the sighting of the supernova, the nebula has been expanding at a rate that roughly corresponds to its age.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Synchrotron Radiation: the Crab Nebula" align="left"/>About 6500 years ago, a star in the constellation of Taurus exploded as a supernova. On July 4, 1054 CE, light from this explosion reached the Earth and was observed by Chinese astronomers, who made a record of their observation. The Crab Nebula has been identified as the detritus from the explosion; and in the approximately 960 years since the sighting of the supernova, the nebula has been expanding at a rate that roughly corresponds to its age.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154304Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryDuration of Synchrotron Radiation in a Typical Supernova Remnant
https://www.maplesoft.com/applications/view.aspx?SID=154305&ref=Feed
Find an estimate for the length of time a typical supernova remnant can radiate, given its magnetic field strength.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Duration of Synchrotron Radiation in a Typical Supernova Remnant" align="left"/>Find an estimate for the length of time a typical supernova remnant can radiate, given its magnetic field strength.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154305Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryRadio-Band and B-Band Luminosity and Brightness of Galaxy NGC 5236
https://www.maplesoft.com/applications/view.aspx?SID=154306&ref=Feed
Compare the radio and B-band intensity with the radio and B-band luminosity of the galaxy NGC 5236.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Radio-Band and B-Band Luminosity and Brightness of Galaxy NGC 5236" align="left"/>Compare the radio and B-band intensity with the radio and B-band luminosity of the galaxy NGC 5236.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154306Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryCalculating and Graphing the Bremsstrahlung Emission Over All Frequencies for the Orion Nebula
https://www.maplesoft.com/applications/view.aspx?SID=154307&ref=Feed
Calculate and graph the bremsstrahlung emission over all frequencies for the Orion Nebula.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Calculating and Graphing the Bremsstrahlung Emission Over All Frequencies for the Orion Nebula" align="left"/>Calculate and graph the bremsstrahlung emission over all frequencies for the Orion Nebula.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154307Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberrySirius A
https://www.maplesoft.com/applications/view.aspx?SID=154308&ref=Feed
Sirius A (Alpha Canis Majoris) is close enough to Earth for accurate parallax measurement of its distance. This knowledge enables an accurate determination of its luminosity. Calculate its (A) mass, (B) radius, and (C) effective temperature, assuming (correctly) that it is a Main Sequence star with mass near that of the Sun.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Sirius A" align="left"/>Sirius A (Alpha Canis Majoris) is close enough to Earth for accurate parallax measurement of its distance. This knowledge enables an accurate determination of its luminosity. Calculate its (A) mass, (B) radius, and (C) effective temperature, assuming (correctly) that it is a Main Sequence star with mass near that of the Sun.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154308Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryGraphing the Planck Function
https://www.maplesoft.com/applications/view.aspx?SID=154309&ref=Feed
Make a plot of the Planck function for temperatures of 2000 K, 3000 K, 4000 K, 5000 K, 6000K, and 7000 K<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Graphing the Planck Function" align="left"/>Make a plot of the Planck function for temperatures of 2000 K, 3000 K, 4000 K, 5000 K, 6000K, and 7000 K<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154309Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryThe Sun
https://www.maplesoft.com/applications/view.aspx?SID=154310&ref=Feed
For the Sun, calculate the (A) central pressure, (B) central temperature, (C) pressure scale height, (D) adiabatic sound speed for a monatomic gas, and (E) the adiabatic convection by Mixing-length Theory<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="The Sun" align="left"/>For the Sun, calculate the (A) central pressure, (B) central temperature, (C) pressure scale height, (D) adiabatic sound speed for a monatomic gas, and (E) the adiabatic convection by Mixing-length Theory<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154310Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryCalculating the Zeeman Effect
https://www.maplesoft.com/applications/view.aspx?SID=154311&ref=Feed
The Ap star BD+0°4535 has a powerful magnetic field of 2.1 T. Calculate the wavelengths of the H[alpha]
line caused by Zeeman splitting.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Calculating the Zeeman Effect" align="left"/>The Ap star BD+0°4535 has a powerful magnetic field of 2.1 T. Calculate the wavelengths of the H[alpha]
line caused by Zeeman splitting.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154311Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryInverse Compton Scattering
https://www.maplesoft.com/applications/view.aspx?SID=154312&ref=Feed
Consider an interstellar cloud of non-relativistic electrons at a temperature T. A large quantity of photons from the Cosmic Microwave Background with energies hν << kT flow continuously through the cloud.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Inverse Compton Scattering" align="left"/>Consider an interstellar cloud of non-relativistic electrons at a temperature T. A large quantity of photons from the Cosmic Microwave Background with energies hν << kT flow continuously through the cloud.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154312Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryThomson Cross Section
https://www.maplesoft.com/applications/view.aspx?SID=154313&ref=Feed
(A) Calculate the Thomson Cross Section and give its value. (B) Which has the greater cross section: electrons or protons? Why? (C) What effect does wavelength have on Thomson scattering? (D) Calculate the optical depth to Thomson scattering in the warm, neutral (HI) medium of the Galactic ISM, normal to the disk. (E) How might Thomson scattering be used to reveal a hidden active galactic nucleus?<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Thomson Cross Section" align="left"/>(A) Calculate the Thomson Cross Section and give its value. (B) Which has the greater cross section: electrons or protons? Why? (C) What effect does wavelength have on Thomson scattering? (D) Calculate the optical depth to Thomson scattering in the warm, neutral (HI) medium of the Galactic ISM, normal to the disk. (E) How might Thomson scattering be used to reveal a hidden active galactic nucleus?<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154313Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryDoppler Broadening
https://www.maplesoft.com/applications/view.aspx?SID=154314&ref=Feed
Calculate the Doppler broadening of the iron lines at the surface of the Sun.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Doppler Broadening" align="left"/>Calculate the Doppler broadening of the iron lines at the surface of the Sun.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154314Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert RoseberryLine Broadening Due to Heisenberg's Uncertainty Principle
https://www.maplesoft.com/applications/view.aspx?SID=154315&ref=Feed
Quantum effects based on the Uncertainty Principle cause a line damping profile known as a Lorentzian or Cauchy profile. This type of broadening is called natural broadening and is typically much smaller than Doppler broadening or pressure broadening, which are usually more significant in astrophysical objects. Find the amount of broadening due to the Uncertainty Principle.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.<img src="/applications/images/app_image_blank_lg.jpg" alt="Line Broadening Due to Heisenberg's Uncertainty Principle" align="left"/>Quantum effects based on the Uncertainty Principle cause a line damping profile known as a Lorentzian or Cauchy profile. This type of broadening is called natural broadening and is typically much smaller than Doppler broadening or pressure broadening, which are usually more significant in astrophysical objects. Find the amount of broadening due to the Uncertainty Principle.<BR><BR>For more information on how to do this problem, and for tables of relevant data, see <A HREF="http://www.canismajor.ca">www.canismajor.ca</A>.154315Mon, 25 Sep 2017 04:00:00 ZDr. Robert RoseberryDr. Robert Roseberry