vodcast 5 2 energy levels ipad

00:16:11
https://www.youtube.com/watch?v=noA7GVQlslo

Summary

TLDRLa conferència aborda el tema dels nivells d'energia a través del model de Bohr, conegut com el model planetari, on els electrons orbiten el nucli en trajectòries fixes. A més, se centra en l'estudi de l'espectroscòpia, que permet analitzar els espectres de llum emesos pels elements quan se'ls aplica energia. Aquest fenomen, conegut com l'espectre d'emissió, revela línies distintives que es poden utilitzar per identificar elements, similar a una empremta digital. El vídeo també introdueix conceptes fonamentals com la longitud d'ona i la freqüència, claus per entendre les relacions entre energia i espectre electromagnètic. Finalment, es discuteix el model modern de l'àtom i l'impacte de la freqüència en el càlcul de l'energia emesa, i es presenten fórmules matemàtiques bàsiques per a aquests càlculs.

Takeaways

  • 🔬 El model de Bohr s'explica com un sistema planetari amb electrons orbitant el nucli.
  • 🌈 L'espectroscòpia és l'estudi de l'espectre de llum d'elements escalfats.
  • 💡 Els espectres d'emissió són únics per a cada element, similar a una empremta digital.
  • 📏 La longitud d'ona representa la distància entre dos punts iguals en ones consecutives.
  • 📊 La freqüència és el nombre de cicles d'ona que passen per un punt en un segon.
  • 🧪 Les línies espectrals ajuden a identificar elements a distància, útil en astronomia.
  • 💥 El model de Bohr es complica amb elements amb múltiples electrons.
  • 📉 Les ones electromagnètiques inclouen llum visible, infraroja i ultraviolada.
  • ➗ Fórmules simples relacionen longitud d'ona, freqüència i energia.
  • 🪐 El model modern de l'àtom incorpora un núvol electrònic més complex.

Timeline

  • 00:00:00 - 00:05:00

    En la primera part del vídeo, es discuteix el model de Bohr de l'àtom, conegut també com el model planetari. Aquest model descriu els electrons orbitant el nucli de manera similar a com els planetes orbiten el sol. Cada òrbita s'etiqueta amb els números 1, 2, 3, etc. Després, s'introdueix el concepte de nivells d'energia i es comença a parlar sobre l'espectroscòpia, que implica analitzar com la llum es descompon en diferents bandes de color quan passa per un prisma. Es proporciona un exemple amb l'emissió de llum de l'hidrogen quan s'excita amb energia.

  • 00:05:00 - 00:10:00

    En el segon segment, s'explica més a fons el concepte de l'espectre d'emissió, fent èmfasi en com cada element té un espectre únic que actua com una empremta digital. Això permet als científics identificar elements i compostos, fins i tot en planetes distants, mitjançant l'observació dels seus espectres. Es detallen els conceptes d'estat fonamental i excitat dels electrons, i com el retorn dels electrons a l'estat fonamental després de ser excitats resulta en l'emissió de radiació electromagnètica, incloent la llum visible.

  • 00:10:00 - 00:16:11

    Finalment, en la tercera part, es descriuen els conceptes de longitud d'ona i freqüència. La longitud d'ona és la distància entre dos pics consecutius d'una ona. La freqüència, que es mesura en Hertz, indica quantes vegades passa una longitud d'ona per un punt en un segon. S'explica la relació inversa entre longitud d'ona i freqüència i es presenten fórmules matemàtiques per calcular aquestes variables. A més, es descriuen els càlculs per determinar l'energia a través de la constant de Planck i es demostra com aquestes fórmules ajuden a entendre els nivells d'energia en el model de Bohr.

Mind Map

Mind Map

Faqs

  • Què és el model de Bohr de l'àtom?

    El model de Bohr representa l'àtom de manera que els electrons circulen al voltant del nucli en òrbites específiques, similars als planetes que orbiten al voltant del sol.

  • Què és l'espectroscòpia?

    L'espectroscòpia és l'estudi dels espectres de llum que emeten els àtoms o elements quan se'ls aplica energia.

  • Com es forma l'espectre d'emissió?

    Quan un àtom s'excita aplicant-li energia, els electrons salten a nivells d'energia superiors i, en tornar als nivells interiors, emeten radiació en forma de llum visible creant un espectre d'emissió.

  • Què representa cada línia a l'espectre d'emissió?

    Cada línia de l'espectre d'emissió representa una longitud d'ona específica que es pot associar a la transició dels electrons entre nivells d'energia en un àtom.

  • Per què el model de Bohr no funciona amb elements amb més d'un electró?

    El model de Bohr es complica amb elements amb més d'un electró perquè les interaccions elèctriques entre electrons provoquen sistemes molt més complexos.

  • Què són el període i la freqüència de les ones?

    El període és el temps que triga una ona a completar un cicle complet, mentre que la freqüència és el nombre de cicles que passen per un punt per unitat de temps.

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  • 00:00:01
    all right guys let's get into some super
  • 00:00:03
    crazy stuff here we're going to uh start
  • 00:00:05
    broadcast 5.2 um where we're going to be
  • 00:00:07
    talking um about energy levels um and
  • 00:00:10
    what that means is that if we look at a
  • 00:00:13
    boore model of the atom okay so if you
  • 00:00:16
    recall um back when we did our little
  • 00:00:19
    bit on development of atomic theory that
  • 00:00:21
    the Board model um was in general
  • 00:00:24
    called the planetary model OKAY was
  • 00:00:28
    called the planetary model because we've
  • 00:00:30
    got these orbits okay in which electrons
  • 00:00:33
    okay so this electron are circling the
  • 00:00:36
    nucleus kind of like planets are
  • 00:00:38
    circling the Sun and they're in these
  • 00:00:39
    very specific orbits so there's an orbit
  • 00:00:42
    here and one here and one here and here
  • 00:00:44
    and then so on and so forth and bore
  • 00:00:46
    labels each of these Nal 1 2 3 4 5 six
  • 00:00:50
    7even okay on all the way out um and so
  • 00:00:55
    nucleus in the middle that's where the
  • 00:00:56
    protons and neutrons are electrons are
  • 00:00:58
    then in these orbits okay so that's the
  • 00:01:01
    essential bore model what we're going to
  • 00:01:03
    see here is what's important is these
  • 00:01:04
    energy levels and what happens with the
  • 00:01:07
    interaction um between things with these
  • 00:01:09
    energy levels okay so let's jump over to
  • 00:01:13
    our next slide here and see something
  • 00:01:15
    that looks really different than
  • 00:01:16
    anything we've seen before um this all
  • 00:01:18
    has to do with something called
  • 00:01:20
    spectroscopy U and what spectroscopy
  • 00:01:22
    means is and it's pretty easy but
  • 00:01:24
    spectroscopy has to do with Spectrum
  • 00:01:27
    okay you guys have all seen um light it
  • 00:01:29
    goes through a prism and it splits up
  • 00:01:31
    and sort of forms a rainbow um well you
  • 00:01:33
    can do that too with atoms um with
  • 00:01:36
    specific elements um and so I'm going to
  • 00:01:38
    show you a short little video clip here
  • 00:01:40
    um that represents this right here which
  • 00:01:42
    is a hydrogen gas in a tube and
  • 00:01:45
    basically if you apply a lot of energy
  • 00:01:46
    to it that hydrogen gas is going to glow
  • 00:01:49
    and it's going to emit light if you then
  • 00:01:51
    pass that light through these slits you
  • 00:01:53
    can separated out into these different
  • 00:01:56
    bands okay so we're going to take a
  • 00:01:58
    quick pause and watch that video clip
  • 00:01:59
    and then we'll come come back here to
  • 00:02:01
    okay so real quick this is the hydrogen
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    Spectrum notice it's making a loud
  • 00:02:05
    buzzing that's the uh electricity going
  • 00:02:07
    in there we're going to put a
  • 00:02:08
    spectroscope up to this and if you look
  • 00:02:10
    real close you can see some of these
  • 00:02:11
    sharp little lines that we're talking
  • 00:02:13
    about so here comes the spectroscope no
  • 00:02:15
    it's kind of hard to see because I got a
  • 00:02:16
    camera over you see those sharp lines
  • 00:02:18
    that's what we're looking for those are
  • 00:02:20
    the
  • 00:02:22
    Spectrum this
  • 00:02:26
    part okay so what what we saw there was
  • 00:02:30
    that and you couldn't really see it in
  • 00:02:31
    the video because again I'm trying to
  • 00:02:32
    look through a spectroscope with a
  • 00:02:34
    camera which doesn't work terribly well
  • 00:02:36
    um but what happens there is that you
  • 00:02:38
    start to see these very distinct lines
  • 00:02:40
    of very distinct colors um this is
  • 00:02:42
    what's called an emission spectrum okay
  • 00:02:45
    um there's different kinds of spectrum
  • 00:02:46
    you can do absorption uh Spectrum where
  • 00:02:48
    basically this is reversed but this is
  • 00:02:50
    called an emission spectrum and this is
  • 00:02:51
    if you look down here um this is the
  • 00:02:55
    wavelength okay what we're measuring in
  • 00:02:58
    each P place is the wavelength length of
  • 00:03:00
    that energy we're going to talk a little
  • 00:03:02
    bit more about wavelength here in a
  • 00:03:03
    second okay but the idea is that every
  • 00:03:07
    element okay has a specific emission
  • 00:03:09
    Spectra that if you excite it if you
  • 00:03:11
    heat it up then it's going to give off
  • 00:03:13
    these certain ways of light now the
  • 00:03:15
    whole reason for this and bore is the
  • 00:03:17
    guy that discovers the reason for this
  • 00:03:19
    because they' known about emission
  • 00:03:20
    spectrum for a while what they didn't
  • 00:03:22
    really know is why it was happening in a
  • 00:03:24
    specific way and why certain elements
  • 00:03:26
    gave off these certain patterns so if we
  • 00:03:28
    look right here here and what is called
  • 00:03:31
    the Balmer
  • 00:03:32
    series okay you see that there are four
  • 00:03:35
    lines here 410 434 486 656 nanometers
  • 00:03:40
    those lines correspond to these colors
  • 00:03:45
    okay these bands of color that we get
  • 00:03:47
    when we excite the hydrogen now so the
  • 00:03:49
    question is then what is going on there
  • 00:03:52
    um in those bands well here's what
  • 00:03:54
    happens so in the boore model there's
  • 00:03:56
    these energy levels right 1 two 3 4 five
  • 00:04:00
    six so on and so forth what happens is
  • 00:04:03
    that in a normal hydrogen atom okay the
  • 00:04:06
    electron is down here in n equals 1 okay
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    in under normal circumstances if we put
  • 00:04:12
    energy in it jumps up out of that level
  • 00:04:15
    into higher levels it becomes what we
  • 00:04:17
    call an excited electron okay and
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    excited just means that it's not in the
  • 00:04:23
    normal energy level okay that it's
  • 00:04:25
    higher up than its ground state so any
  • 00:04:28
    of these for hydrogen would the excited
  • 00:04:30
    levels if an electron was down here at
  • 00:04:32
    the bottom um we would call that the
  • 00:04:36
    ground state okay so that's its normal
  • 00:04:38
    position and if we put energy in it gets
  • 00:04:40
    excited now once it gets excited they're
  • 00:04:43
    going to start to fall back down and
  • 00:04:44
    when they fall back down they emit
  • 00:04:46
    radiation okay electromagnetic radiation
  • 00:04:49
    and if they emit it in this range okay
  • 00:04:52
    right here this is what's called visible
  • 00:04:54
    light and that's the part that we can
  • 00:04:55
    actually see you can see that there are
  • 00:04:57
    parts of it that are emitted outside of
  • 00:05:00
    visible light okay so we got infrared
  • 00:05:02
    over here and UltraViolet over here so
  • 00:05:04
    we can detect those as well but the part
  • 00:05:06
    that we're really interested in is the
  • 00:05:08
    spectroscopy that gives us this very
  • 00:05:10
    specific Spectrum okay um every element
  • 00:05:15
    um essentially and a lot of compounds as
  • 00:05:17
    well have very distinct spectrum that
  • 00:05:20
    they give if you ever wondered like
  • 00:05:21
    where astronomers like you know they say
  • 00:05:24
    hey we found um a planet and its
  • 00:05:26
    atmosphere we believe is mostly methane
  • 00:05:28
    or something like that and you're like
  • 00:05:30
    well how the heck do they know that the
  • 00:05:31
    atmosphere is methane I mean they they
  • 00:05:34
    not like they've been to that planet and
  • 00:05:35
    sampled it they know because of
  • 00:05:37
    spectroscopy they can look at it with
  • 00:05:38
    specific instruments they can see these
  • 00:05:41
    bands and every element and most
  • 00:05:44
    compounds um have a very specific band
  • 00:05:47
    kind of like a
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    fingerprint um for an element or a
  • 00:05:51
    compound okay so
  • 00:05:54
    specific okay to an element okay or a
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    compound for that matter
  • 00:06:00
    um and it's like a
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    fingerprint okay so it's sort of a
  • 00:06:05
    unique identifier and indeed this is one
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    of the ways that they like if you do
  • 00:06:08
    blood work or something like that that
  • 00:06:10
    they're going to measure say um how much
  • 00:06:13
    maybe potassium is in your blood is
  • 00:06:15
    they're going to take your blood sample
  • 00:06:16
    and they're going to run it through a
  • 00:06:17
    machine but what the machine is actually
  • 00:06:18
    doing is getting one of these emission
  • 00:06:21
    spectrum okay and they can then identify
  • 00:06:24
    the bands and say hey that's potassium
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    and we've got this much of it okay so
  • 00:06:28
    what is this mean to us well first off
  • 00:06:31
    um B's model worked really well for the
  • 00:06:34
    hydrogen atom um but the problem was
  • 00:06:37
    they found out that it didn't work for
  • 00:06:38
    anything else okay and the reason for
  • 00:06:41
    that is that everything else there's
  • 00:06:42
    more than one electron and so things
  • 00:06:44
    started to get really ridiculously
  • 00:06:47
    complicated when you added in extra
  • 00:06:49
    electrons so this over here to the side
  • 00:06:52
    this is the modern model of the atom
  • 00:06:54
    okay and what's going on here is we've
  • 00:06:56
    got a cloud you see this sort of
  • 00:06:57
    fuzziness nucleus is in the middle
  • 00:06:59
    little tiny spot in the middle remember
  • 00:07:00
    Rutherford found out that nucleus was in
  • 00:07:02
    the middle and that it took up hardly
  • 00:07:04
    any space at all and then this fuzzy
  • 00:07:06
    area on the outside that's the electron
  • 00:07:07
    cloud now we're going to talk a lot more
  • 00:07:09
    about what where the electrons actually
  • 00:07:10
    are there in a little bit um but what is
  • 00:07:13
    so what does that have to do with this
  • 00:07:15
    Bard model that we've been talking about
  • 00:07:16
    well let's see if we can relate this to
  • 00:07:18
    energy in the electrons okay so we need
  • 00:07:20
    to learn a couple of quick terms um and
  • 00:07:23
    these terms that are really important to
  • 00:07:24
    us here are wavelength that was some
  • 00:07:27
    awesome circling and frequency okay and
  • 00:07:30
    this is what wavelength is wavelength is
  • 00:07:32
    just what it sounds like it's the length
  • 00:07:34
    of a wave okay light and infrared and
  • 00:07:37
    gamma rays and all that those are part
  • 00:07:38
    of the electromagnetic spectrum okay
  • 00:07:41
    which is radiation and radiation has is
  • 00:07:44
    a wave function we'll talk later that
  • 00:07:46
    it's if you take other science class
  • 00:07:47
    it's not technically just a wave but
  • 00:07:49
    anyway it's a wave function and so the
  • 00:07:51
    length of the wave from one Peak to the
  • 00:07:53
    next Peak is a wavelength or from one
  • 00:07:55
    midpoint to another midpoint is a
  • 00:07:57
    wavelength basically from any one point
  • 00:07:59
    to the exact same point on the next wave
  • 00:08:02
    that's a wavelength we measure it in
  • 00:08:03
    meters or usually considering how small
  • 00:08:05
    they are something like nanometers if
  • 00:08:07
    we're talking about um for if for
  • 00:08:10
    instance if we're talking about uh light
  • 00:08:12
    it's going to be in nanometers and
  • 00:08:13
    that's what those measurements were back
  • 00:08:14
    on the hydrogen Spectrum um the second
  • 00:08:16
    definition is something called frequency
  • 00:08:18
    frequency is basically the inverse
  • 00:08:20
    function of wavelength and frequency if
  • 00:08:23
    you see here on this GIF um frequency is
  • 00:08:25
    how many wavelengths pass a given point
  • 00:08:27
    in a second okay
  • 00:08:29
    um and it's measured in hertz which is
  • 00:08:32
    basically one over second or cycles per
  • 00:08:35
    second okay um Hertz is
  • 00:08:38
    HZ okay and if we had actually had to
  • 00:08:41
    write out the unit it would be one over
  • 00:08:43
    seconds or sometimes you'll see it
  • 00:08:45
    written as this they all mean the same
  • 00:08:47
    thing basically just means how many
  • 00:08:48
    waves pass by in a second and what you
  • 00:08:50
    can see here in this GIF is that uh the
  • 00:08:52
    Herz is going up as the waves get more
  • 00:08:55
    compacted as they get pressed together a
  • 00:08:56
    little bit more um the the frequency is
  • 00:08:59
    going to go up and as they're spread
  • 00:09:01
    apart more so like right now they're
  • 00:09:03
    getting really crunched together then
  • 00:09:04
    the frequency is higher so it's about
  • 00:09:06
    five Hertz there as they're really far
  • 00:09:08
    apart and the Herz is low that means
  • 00:09:10
    that you've got a really big wavelength
  • 00:09:12
    so they're inversely related okay and
  • 00:09:14
    that's going to lead us to a couple of
  • 00:09:16
    math formulas now we're not going to
  • 00:09:18
    work a whole bunch of these we'll work a
  • 00:09:19
    couple in class just because I want you
  • 00:09:20
    to be familiar with them because we may
  • 00:09:22
    see a couple um but we won't stress too
  • 00:09:24
    much about it just make sure that you
  • 00:09:26
    understand what the terms are and how to
  • 00:09:28
    plug stuff in they're just algebra
  • 00:09:29
    equations so here's our first equation
  • 00:09:32
    um it's called the Lambda V equation so
  • 00:09:34
    C equals Lambda V this weird looking
  • 00:09:37
    letter here um is called a Lambda okay
  • 00:09:40
    um and if you're wondering how that's
  • 00:09:42
    spelled okay that is it's a Greek letter
  • 00:09:45
    and it's spelled oh I messed it up l a m
  • 00:09:49
    BDA Lambda okay and so C equals Lambda v
  • 00:09:53
    c is the speed of light if you remember
  • 00:09:55
    um Einstein's equation that we sort of
  • 00:09:57
    see written up all the time the e = mc^2
  • 00:10:01
    it's the same c as in that equation Okay
  • 00:10:04
    C is the speed of light it's uh 3.0 *
  • 00:10:06
    108 meters per second which is really
  • 00:10:09
    fast doesn't I mean it's kind of a big
  • 00:10:11
    number but it doesn't sound like much
  • 00:10:12
    but that is pretty fast it's basically
  • 00:10:14
    as fast as anything we know can go
  • 00:10:16
    unless that neutrino experiment that
  • 00:10:18
    just happened is true um Lambda is the
  • 00:10:19
    wavelength it's usually in meters um if
  • 00:10:22
    it's in anything but meters that you'll
  • 00:10:24
    need to change it and the way it's
  • 00:10:26
    usually going to be written for us is
  • 00:10:27
    nanometers um so we sort of need an
  • 00:10:30
    equality there and the way that works is
  • 00:10:31
    that um 1 meter equal 10 9th nanometers
  • 00:10:37
    or basically a billion nanometers okay
  • 00:10:41
    and V is in frequency we already said
  • 00:10:42
    that that's in hertz or in one over
  • 00:10:45
    seconds okay so we're going to work a
  • 00:10:47
    real quick problem here just so we can
  • 00:10:48
    see how this works and we'll work one
  • 00:10:49
    more equation after this probably so
  • 00:10:52
    what is a frequency of red light with a
  • 00:10:53
    wavelength of 656 NM so as soon as you
  • 00:10:57
    see that um you should immediately
  • 00:10:59
    convert your nanometers into meters now
  • 00:11:03
    there's a couple of ways that you could
  • 00:11:04
    do that you could use the staircase and
  • 00:11:06
    move it nine spaces which might actually
  • 00:11:08
    be easier or you can do a real quick
  • 00:11:11
    conversion factor just like this okay if
  • 00:11:15
    we calculate this out whoops I totally
  • 00:11:17
    wrote that wrong didn't I 56 we're going
  • 00:11:19
    to get
  • 00:11:21
    6.56 * 10
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    the7th m okay now that is my Lambda
  • 00:11:29
    value okay
  • 00:11:32
    Lambda so our equation then remember is
  • 00:11:35
    C equals Lambda
  • 00:11:38
    V okay I know Lambda C is a constant
  • 00:11:41
    it's always 3.0 * 108 so we're just
  • 00:11:45
    going to plug this stuff
  • 00:11:46
    in time 10 and that's to the e8th not
  • 00:11:49
    negative e meters per second
  • 00:11:52
    equals
  • 00:11:55
    6.5 that is some bad handwriting Arnold
  • 00:11:59
    okay
  • 00:12:02
    6.56 *
  • 00:12:04
    107 M that's what we just found up here
  • 00:12:07
    okay that goes right in there and that's
  • 00:12:09
    times V and V of course is what I'm
  • 00:12:12
    looking for okay so we're going to punch
  • 00:12:15
    that into the calculator now
  • 00:12:16
    algebraically what do we need to do um
  • 00:12:17
    if I want V by itself which is what I'm
  • 00:12:19
    solving for I'm going to divide both
  • 00:12:21
    sides by the
  • 00:12:25
    wavelength okay so divide both sides by
  • 00:12:28
    that
  • 00:12:30
    and of course you don't actually have to
  • 00:12:31
    necessarily write out this entire step
  • 00:12:34
    of algebra if you're doing this but if
  • 00:12:36
    you're uncomfortable with it that'll
  • 00:12:37
    work so that cancels out this side punch
  • 00:12:40
    this number into our calculator and
  • 00:12:42
    we're going to get
  • 00:12:44
    4.54 okay three sigfigs time 10 14th
  • 00:12:49
    Hertz now what this means really small
  • 00:12:52
    wave length Okay time 10 the -7th M okay
  • 00:12:57
    means really big frequency they're
  • 00:12:58
    inverse ly proportional now why was that
  • 00:13:01
    important what did that have to do with
  • 00:13:02
    the Bor mod it has to do with this
  • 00:13:03
    because once we know
  • 00:13:05
    frequency we can then calculate the
  • 00:13:07
    energy and why do we care about energy
  • 00:13:09
    because if I go back several slides okay
  • 00:13:14
    the energy is what's given off here okay
  • 00:13:17
    and the energy then leads to these
  • 00:13:19
    frequencies so for each of these
  • 00:13:20
    individual frequencies we could or um
  • 00:13:23
    wavelengths we could calculate the
  • 00:13:25
    frequency and then turn those into
  • 00:13:27
    energy using these two equations and
  • 00:13:29
    that's exactly what scientists do okay
  • 00:13:32
    so real quick let me work one of these
  • 00:13:33
    equations equation itself pretty easy
  • 00:13:35
    energy is equal to H time v um e is
  • 00:13:38
    energy in Jewels V is the frequency that
  • 00:13:40
    we had in the last equation and H is a
  • 00:13:43
    constant it's called planks constant and
  • 00:13:45
    it's this is its number super small
  • 00:13:48
    number that's a smaller number than
  • 00:13:50
    aag's number is Big 6.62 6 time 10 34th
  • 00:13:54
    really tiny number we did one of those
  • 00:13:57
    back in scientific notation time
  • 00:13:59
    okay so real quick let's work one of
  • 00:14:01
    these problems um it won't take us too
  • 00:14:02
    long so let's just crank one out so E
  • 00:14:05
    equals
  • 00:14:06
    HV okay I guess we should read the
  • 00:14:08
    problem first given a frequency of 1.60
  • 00:14:11
    * 10 15th Hertz what is the energy of
  • 00:14:13
    this particle so I'm looking for energy
  • 00:14:15
    energy is e okay I'm given frequency
  • 00:14:18
    frequency is V and H is a constant okay
  • 00:14:23
    remember that's from the last slide so H
  • 00:14:26
    is equal to
  • 00:14:27
    6.62 6 * 10
  • 00:14:32
    34th okay you might not have noticed the
  • 00:14:35
    ules the units on it the ules the units
  • 00:14:37
    it's jewles times seconds and the reason
  • 00:14:39
    for that is that remember Hertz is one
  • 00:14:42
    over seconds so when we multiply This
  • 00:14:44
    Together the seconds cancel and we're
  • 00:14:45
    left with jewels and that's exactly what
  • 00:14:47
    we want to happen so this one's even
  • 00:14:48
    more straightforward than the last one
  • 00:14:50
    because I'm just going to plug it in and
  • 00:14:51
    then punch stuff into my calculator so
  • 00:14:53
    6.
  • 00:14:55
    626 * 10 to the negative sorry about
  • 00:14:58
    these negative signs I know I'm B- 34
  • 00:15:01
    Jew time seconds okay and that's
  • 00:15:04
    multiplied by our frequency that's given
  • 00:15:07
    to us in the problem
  • 00:15:09
    1.60 * 10 15 and you don't even have to
  • 00:15:12
    do algebra for this problem okay
  • 00:15:15
    remember that Hertz is one over second
  • 00:15:17
    so that's going to mean that seconds are
  • 00:15:19
    going to cancel and we're just going to
  • 00:15:21
    be left with
  • 00:15:22
    jewels you just punch that into the
  • 00:15:24
    calculator there's no real algebra that
  • 00:15:25
    needs to and you just got to do the math
  • 00:15:27
    punch it in the calculator so 1.06 * 10
  • 00:15:31
    to the
  • 00:15:32
    Nega
  • 00:15:34
    negative
  • 00:15:36
    18th Jewels okay let me clean that up
  • 00:15:39
    just a little bit because I know that's
  • 00:15:40
    a little hard to see okay so negative
  • 00:15:43
    18th Jewels that's a pretty small number
  • 00:15:46
    um and it should be I mean we're talking
  • 00:15:47
    about one little particle okay one
  • 00:15:50
    electron moving one energy level in one
  • 00:15:52
    atom could to be a pretty small amount
  • 00:15:54
    obviously if that happens in a lot of
  • 00:15:55
    them then that becomes a much bigger
  • 00:15:57
    amount okay we're probably not going to
  • 00:15:59
    do a a a massive ton of these
  • 00:16:01
    calculations but we'll work through four
  • 00:16:02
    or five in class just to make sure we
  • 00:16:04
    know how to do this and then we'll move
  • 00:16:05
    on in the next section to the real
  • 00:16:06
    important stuff which is electron
  • 00:16:09
    configurations thanks guys
Tags
  • model de Bohr
  • espectroscòpia
  • nivells d'energia
  • espectre d'emissió
  • longitud d'ona
  • freqüència
  • ràdio electromagnètic