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      <title>GR12 EMISSION SPECTRA (PHOTOELECTRIC EFFECT - SECTION 2) by Lizelle Swanepoel</title>
      <link>https://padlet.com/lizellexs/owo3nqsq49cj</link>
      <description></description>
      <language>en-us</language>
      <pubDate>2018-09-19 20:43:38 UTC</pubDate>
      <lastBuildDate>2023-08-28 18:11:56 UTC</lastBuildDate>
      <webMaster>hello@padlet.com</webMaster>
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         <title></title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283648096</link>
         <description><![CDATA[]]></description>
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         <pubDate>2018-09-19 20:46:27 UTC</pubDate>
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         <title></title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283648214</link>
         <description><![CDATA[]]></description>
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         <pubDate>2018-09-19 20:46:51 UTC</pubDate>
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         <title></title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283648390</link>
         <description><![CDATA[]]></description>
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         <pubDate>2018-09-19 20:47:35 UTC</pubDate>
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         <title>What is the difference between absorption and emission spectra?</title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283652708</link>
         <description><![CDATA[]]></description>
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         <pubDate>2018-09-19 21:05:24 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283652708</guid>
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      <item>
         <title>CONTINUOUS EMISSION SPECTRUM FROM WHITE LIGHT</title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283799441</link>
         <description><![CDATA[<div>THIS IS WHERE IT ALL STARTED...</div><ul><li>In 1666, Isaac Newton discovered that white light can be separated into its component colours using glass prisms. </li><li>The spectrum produced is a continuous spectrum</li><li>Continuous spectra are produced by HOT DENSE GASES LIKE THE SUN.</li></ul><div><br></div>]]></description>
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         <pubDate>2018-09-20 09:35:59 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283799441</guid>
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         <title>After Newton&#39;s discovery, scientists were using this new tool to analyze the light coming from several different light sources. </title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283800082</link>
         <description><![CDATA[<div>- Some scientists looked at hot objects and gases; <br>- Others looked at the stars. <br>- Observations were made and patterns detected. </div>]]></description>
         <enclosure url="" />
         <pubDate>2018-09-20 09:38:10 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283800082</guid>
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         <title>Element: Unique Signature</title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283800386</link>
         <description><![CDATA[<div>Every element emits a unique range of colours called spectral lines. <br><strong>Spectral lines</strong>:</div><ul><li>identify atoms/molecules</li><li>identify the components of stars</li><li>are dark or bright lines in an otherwise continuous spectrum </li><li>  result from emission or absorption of light in a narrow frequency range.</li></ul><div><br></div><div><strong><mark>A spectrum is produced when light shines through a gas</mark></strong>; </div><ul><li>Certain colours, or wavelengths, are absorbed by the gas </li><li>which produces a pattern of colours and dark lines called an <mark>absorption spectrum.</mark></li><li>The "photographic negative" of an absorption spectrum is an <mark>emission spectrum</mark>.</li></ul>]]></description>
         <enclosure url="" />
         <pubDate>2018-09-20 09:39:14 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283800386</guid>
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      <item>
         <title></title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283800859</link>
         <description><![CDATA[]]></description>
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         <pubDate>2018-09-20 09:41:07 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283800859</guid>
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         <title>Scientists use spectra to analyze unknown substances. </title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283801034</link>
         <description><![CDATA[]]></description>
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         <pubDate>2018-09-20 09:41:50 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283801034</guid>
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         <title>The Light from Stars Contains Information </title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283801264</link>
         <description><![CDATA[<div><br>- The core of a star is HOT (15×10<sup>6</sup>K), and GLOWS. <br>- Astronomers can learn about a star’s motion, temperature, composition by analyzing starlight that reaches Earth. <br>- A <strong><mark>spectroscope</mark></strong> is used to analyze light from stars and other sources:  </div><ul><li> It separates light into a spectrum.</li><li>The light directed from a telescope through a spectroscope<strong> </strong>produces an image called a <strong><mark>spectrograph</mark></strong>. </li></ul>]]></description>
         <enclosure url="" />
         <pubDate>2018-09-20 09:42:29 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/283801264</guid>
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      <item>
         <title></title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/284133936</link>
         <description><![CDATA[]]></description>
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         <pubDate>2018-09-20 20:07:15 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/284133936</guid>
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         <title>VIDEO EXPLAINING EMISSION AND ABSORPTION SPECTRA </title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/284623565</link>
         <description><![CDATA[]]></description>
         <enclosure url="https://youtu.be/xhaDuAkpF8A" />
         <pubDate>2018-09-22 12:05:01 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/284623565</guid>
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      <item>
         <title>EXERCISE with answers</title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/284630538</link>
         <description><![CDATA[<div><strong>1.</strong>&nbsp; &nbsp; &nbsp;<br><strong><mark>Explain how atomic emission spectra arise and how they relate to each element on the periodic table.</mark></strong></div><div>&nbsp;Atomic emission spectra arise from:<br>- Electrons dropping from higher energy levels to lower energy levels within the atom.<br>- Photons (light packets) with specific wavelengths are released, by the formula <strong><mark>E = hf</mark></strong><br>So:&nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;<strong>f</strong> = <strong>ΔE/h</strong>&nbsp; or <strong><mark>c/λ = ΔE/h </mark></strong><br>- The energy levels in an atom are unique to each element on the periodic table.&nbsp;<br>- Therefore the wavelength of light emitted can be used to determine which element the light came from.</div><div><strong>2.</strong>&nbsp; &nbsp; &nbsp;<br><strong><mark>How do the lines on the atomic spectrum relate to electron transitions between energy levels?</mark></strong></div><div>The lines on the atomic spectrum relate to electron transitions between energy levels.<br>Emission lines:<br>- the electron drops an energy level&nbsp;<br>- a photon is released&nbsp;<br>- resulting in an emission line.&nbsp;<br>Absorption lines:<br>- if the electron absorbs a photon it rises an energy level&nbsp;<br>- an absorption line is observed on the spectrum.</div><div>&nbsp;</div><div><strong>3.</strong>&nbsp; &nbsp; &nbsp;<br><strong><mark>Explain the difference between atomic absorption and emission spectra.</mark></strong></div><div>The difference between absorption and emission spectra are that:<br>- <mark>absorption lines</mark> are where light has been absorbed by the atom <br>- thus you see <strong><mark>a dip in the spectrum</mark></strong> <br>- <mark>emission spectra</mark> have <strong><mark>spikes in the spectra</mark></strong>&nbsp;<br>- due to atoms releasing photons at those wavelengths.</div><div>&nbsp;</div><div><strong>4.</strong>&nbsp; &nbsp; &nbsp;<br><strong><mark>Describe how the absorption and emission spectra of the gases in the atmosphere give rise to the Greenhouse Effect.</mark></strong></div><div>The following needs to be in your answer: <br>- in what wavelength range the sunlight reaches the earth, <br>- the absorption of the sunlight <br>- and the re-radiation as <mark>infrared light = HEAT</mark>&nbsp;<br>- the scattering of the infrared light by the carbon-dioxide&nbsp;<br>- how this scattering contributes to the Greenhouse Effect.</div><div><strong>&nbsp;</strong></div><div><strong>5.</strong>&nbsp; &nbsp; &nbsp;<br><strong>What colour is the light emitted by hydrogen when an electron makes the transition from energy level 5 down to energy level 2?&nbsp;</strong></div><div><strong>(Use </strong><a href="https://www.siyavula.com/read/science/grade-12/optical-phenomena-and-properties-of-matter/12-optical-phenomena-and-properties-of-matter-03#fig:Henergy"><strong>Figure 1</strong></a><strong> above to find the energy of the released photon.)</strong></div><div><strong>&nbsp;</strong></div><div>ΔE&nbsp; &nbsp; &nbsp; = E<sub>5</sub> − E<sub>2 </sub>&nbsp; &nbsp; &nbsp; <br>&nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;= 21,0 × 10<sup>−19</sup> − 16,3×10<sup>−19</sup> J&nbsp; &nbsp; &nbsp; &nbsp;<br>&nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;= 4,7 × 10<sup>−19</sup> J &nbsp;<br>&nbsp; &nbsp; &nbsp; &nbsp; &nbsp; (MUST GET POSITIVE ANSWER OUT FOR EMISSION)</div><div>&nbsp;<br>&nbsp;λ&nbsp; &nbsp; &nbsp; &nbsp;= hc/ΔE</div><div>&nbsp; &nbsp; &nbsp; &nbsp; &nbsp; = (6,63×10<sup>−34</sup>)(3×10<sup>8</sup>) / 4,7×10<sup>−19</sup>&nbsp;</div><div>&nbsp; &nbsp; &nbsp; &nbsp; &nbsp; = 423 nm&nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; <br>Colour of light emitted at <strong><mark>423 nm is violet</mark></strong>.</div><div><strong>6.</strong>&nbsp; &nbsp; &nbsp;<br><strong>I have a glass tube filled with hydrogen gas and shine white light onto the tube. The spectrum I then measure has an emission line at a wavelength of 474 nm. Between which two energy levels did the transition occur?&nbsp;</strong></div><div><strong>(Use </strong><a href="https://www.siyavula.com/read/science/grade-12/optical-phenomena-and-properties-of-matter/12-optical-phenomena-and-properties-of-matter-03#fig:Henergy"><strong>Figure </strong></a><strong>2&nbsp; in solving the problem.)</strong></div><div><strong>&nbsp;</strong></div><div>ΔE&nbsp; &nbsp; &nbsp; = hc / λ</div><div>&nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;= (6,63×10<sup>−34</sup>)(3×10<sup>8</sup> ) / 474×10<sup>−9</sup> <br>&nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;= 4,20×10<sup>−19</sup> J&nbsp; &nbsp; &nbsp; &nbsp; &nbsp;<br>Transition occurred from E-level 4 to E-level 2.</div><div>&nbsp;</div>]]></description>
         <enclosure url="" />
         <pubDate>2018-09-22 13:19:17 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/284630538</guid>
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         <title>EMISSION SPECTRA = The Signature of the Stars</title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/284631098</link>
         <description><![CDATA[]]></description>
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         <pubDate>2018-09-22 13:24:58 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/284631098</guid>
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         <title>Transitions in Hydrogen - Fig. 1</title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/284641092</link>
         <description><![CDATA[]]></description>
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         <pubDate>2018-09-22 14:55:55 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/284641092</guid>
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         <title>Spectrum Demo</title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/285368937</link>
         <description><![CDATA[]]></description>
         <enclosure url="https://youtu.be/oae5fa-f0S0" />
         <pubDate>2018-09-25 08:03:08 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/285368937</guid>
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         <title>COMPARISON BETWEEN HOW ABSORPTION VS EMISSION LINE SPECTRA FORM</title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/285370357</link>
         <description><![CDATA[]]></description>
         <enclosure url="https://youtu.be/6IMJglnz2Uw" />
         <pubDate>2018-09-25 08:08:17 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/285370357</guid>
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         <title>EXPLANATION</title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/285371910</link>
         <description><![CDATA[]]></description>
         <enclosure url="https://youtu.be/lJh2Ra1eygA" />
         <pubDate>2018-09-25 08:13:45 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/285371910</guid>
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         <title>QUESTIONS WITH ANSWERS</title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/372011575</link>
         <description><![CDATA[<div>PHOTOELECTRIC EFFECT &amp; EMISSION SPECTRA</div>]]></description>
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         <pubDate>2019-07-23 08:58:47 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/372011575</guid>
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      <item>
         <title>BALMER, LYMAN AND PASCHEN SERIES</title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/550469812</link>
         <description><![CDATA[<div>REMEMBER:&nbsp;</div><ul><li>IN EMISSION SPECTRA OUR HUMAN EYE OBSERVE ONLY THE SPECTRA EMITTED WITHIN THE VISIBLE LIGHT EM-RANGE, i.e. <mark>electron transitions</mark> from higher energy levels <mark>down to energy level 2</mark>! This produces the <strong><mark>Balmer series</mark></strong><strong> of radiation.</strong></li><li>There are also <mark>electron transitions all the way back down to energy level 1</mark>, but that process emits UV radiation. UV is out of the scope of our normal eye vision. We need special spectrographs to observe that. This produces the <strong><mark>Lyman series </mark></strong><strong>of radiation.</strong></li><li>There are also <mark>electron transitions down to energy level 3</mark>, but that process emits IR radiation. Infrared (IR) radiation is out of the scope of our normal eye vision. This produces the <strong><mark>Paschen series</mark></strong><strong> of radiation.</strong></li></ul><div><br></div>]]></description>
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         <pubDate>2020-05-04 20:21:36 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/550469812</guid>
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         <title>THE EMISSION LINE SPECTRUM FOR HYDROGEN</title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/550470504</link>
         <description><![CDATA[<div>What does each line represent?<br>How do emission spectra like this prove the quantum model of the atom?</div>]]></description>
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         <pubDate>2020-05-04 20:21:59 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/550470504</guid>
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         <title></title>
         <author>lizellexs</author>
         <link>https://padlet.com/lizellexs/owo3nqsq49cj/wish/2675476743</link>
         <description><![CDATA[]]></description>
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         <pubDate>2023-08-28 17:50:21 UTC</pubDate>
         <guid>https://padlet.com/lizellexs/owo3nqsq49cj/wish/2675476743</guid>
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