How much of a wave function must reside inside event horizon for it to be consumed by the black hole?2019 Community Moderator Election Unicorn Meta Zoo #1: Why another podcast? Announcing the arrival of Valued Associate #679: Cesar Manara 2019 Moderator Election Q&A - QuestionnaireQuantum phenomena near black hole event horizonCan we have a black hole without a singularity?Why can apparent horizon be computed based on its local geometry?How can light enter a black hole if it cannot get out?Falling into a black hole – how can my perspective change from outside-observer to inside-observer?Can any object pass into the event horizon of a black hole and then escape?Thought experiment: ultra-fast outward push inside a black holeBlack hole merger for a distant observerFree falling into the Schwarzschild black hole: two times doubtMagnet pulling/repelling another magnet beyond the event horizon

"My boss was furious with me and I have been fired" vs. "My boss was furious with me and I was fired"

Can I criticise the more senior developers around me for not writing clean code?

Israeli soda type drink

How do I check if a string is entirely made of the same substring?

What was Apollo 13's "Little Jolt" after MECO?

Bayes factor vs P value

A strange hotel

Did the Roman Empire have penal colonies?

Raising a bilingual kid. When should we introduce the majority language?

Why didn't the Space Shuttle bounce back into space as many times as possible so as to lose a lot of kinetic energy up there?

Was Dennis Ritchie being too modest in this quote about C and Pascal?

As an international instructor, should I openly talk about my accent?

Check if a string is entirely made of the same substring

How to not starve gigantic beasts

What is the term for a person whose job is to place products on shelves in stores?

Arriving in Atlanta after US Preclearance in Dublin. Will I go through TSA security in Atlanta to transfer to a connecting flight?

Has a Nobel Peace laureate ever been accused of war crimes?

Why do distances seem to matter in the Foundation world?

Is there any hidden 'W' sound after 'comment' in : Comment est-elle?

What is it called when you ride around on your front wheel?

Older movie/show about humans on derelict alien warship which refuels by passing through a star

Suing a Police Officer Instead of the Police Department

What to do with someone that cheated their way through university and a PhD program?

iOS App Store: Unable to download and update apps due to Terms and Conditions loop, even after agreeing



How much of a wave function must reside inside event horizon for it to be consumed by the black hole?



2019 Community Moderator Election
Unicorn Meta Zoo #1: Why another podcast?
Announcing the arrival of Valued Associate #679: Cesar Manara
2019 Moderator Election Q&A - QuestionnaireQuantum phenomena near black hole event horizonCan we have a black hole without a singularity?Why can apparent horizon be computed based on its local geometry?How can light enter a black hole if it cannot get out?Falling into a black hole – how can my perspective change from outside-observer to inside-observer?Can any object pass into the event horizon of a black hole and then escape?Thought experiment: ultra-fast outward push inside a black holeBlack hole merger for a distant observerFree falling into the Schwarzschild black hole: two times doubtMagnet pulling/repelling another magnet beyond the event horizon










3












$begingroup$


Related to this question in astronomy SE (https://astronomy.stackexchange.com/q/30611/10813) and in particular my attempt to answer it, I started to wonder which fraction of a waveform (for eg a photon) need to be inside event horizon in order to make its escape impossible? As far as I understand, there is infinitesimal, yet non-zero part of every photon inside event horizons even right now.










share|cite|improve this question











$endgroup$
















    3












    $begingroup$


    Related to this question in astronomy SE (https://astronomy.stackexchange.com/q/30611/10813) and in particular my attempt to answer it, I started to wonder which fraction of a waveform (for eg a photon) need to be inside event horizon in order to make its escape impossible? As far as I understand, there is infinitesimal, yet non-zero part of every photon inside event horizons even right now.










    share|cite|improve this question











    $endgroup$














      3












      3








      3





      $begingroup$


      Related to this question in astronomy SE (https://astronomy.stackexchange.com/q/30611/10813) and in particular my attempt to answer it, I started to wonder which fraction of a waveform (for eg a photon) need to be inside event horizon in order to make its escape impossible? As far as I understand, there is infinitesimal, yet non-zero part of every photon inside event horizons even right now.










      share|cite|improve this question











      $endgroup$




      Related to this question in astronomy SE (https://astronomy.stackexchange.com/q/30611/10813) and in particular my attempt to answer it, I started to wonder which fraction of a waveform (for eg a photon) need to be inside event horizon in order to make its escape impossible? As far as I understand, there is infinitesimal, yet non-zero part of every photon inside event horizons even right now.







      quantum-mechanics black-holes wavefunction event-horizon






      share|cite|improve this question















      share|cite|improve this question













      share|cite|improve this question




      share|cite|improve this question








      edited 4 hours ago









      Qmechanic

      108k122011253




      108k122011253










      asked 4 hours ago









      tuomastuomas

      1484




      1484




















          2 Answers
          2






          active

          oldest

          votes


















          5












          $begingroup$

          Introduction



          First of all we need to establish what the question even means (I will restrict all formulas to non-rotating Schwarzschild black holes of mass $M$ for concreteness). There are no bound states of the electromagnetic field near a black hole, even quasi-stationary states of finite wavelength near the photon radius $r = 3GM/c^2$ will decay, a part falling into the black hole, a part to infinity.



          So the question really is about scattering. It turns out that scattering of electromagnetic waves behaves differently based on wavelength. In SI units the wavelength is $lambda = c/(2pi omega)$ and this is also the localization of the photon. For intuition we can picture the photon as a wavepacket localized in a sphere of radius $lambda$. On the other hand, the typical length of the gravitational background is $GM/c^2$. The main parameter that controls the behavior of the scattering is thus the ratio of these lengths $GM/c^2/(c/(2pi omega))$. I will now switch to geometrized $G=c=1$ units and drop a $2pi$ factor, and then the ratio of the wavelength to the size of the black hole is $sim Momega$.




          Large wavelengths



          For $Momega to 0$ the wavelength is much larger than the black hole, "a very small part of the photon is in the black hole". In this limit it can be computed that the total cross-section of an incoming monochromatic, asymptotically planar wave is
          $$sigma = left[4 pi (2 M)^2 right]frac43M^2 omega^2 + mathcalO(omega^3)$$
          It is difficult to interpret the leading-order term as some kind of "overlapping volume" of the wave and the black hole, since that would scale as $M^3omega^3$. However, a sphere of radius $R$ will scatter particles with a cross-section $4 pi R^2$. Taking a wave-packet with a centroid that would be classically absorbed by a rigid sphere of radius $2M$, the factor $4 M^2 omega^2/3$ can be loosely understood as the probability it will actually be absorbed. Quite interestingly, the low-energy photon sees the black hole as a two-dimensional surface interacting with its wave-front rather than a three-dimensional volume.




          Shorter wavelengths



          However, this all changes with increasing frequency/decreasing wavelength. The intermediate regime is impossible to compute analytically, so I just put a plot from Crispino et al. (2007) here (I also recommend the paper for further references):
          enter image description here
          In the plot, $sigma_E^(omega = 0)$ is the low-frequency limit given above, $sigma_E$ is the total cross-section of monochromatic electromagnetic waves (computed numerically), $sigma_S$ is the same for massless scalar waves, and $sigma_O$ is the optical limit which you get from considering photons as point particles
          $$sigma_O = 27 pi M^2$$
          It is now easy to see that once the size of the wavepacket is comparable or smaller than the black hole, you can simply use the following approximate intuition: If the wavepacket centroid is within the photon sphere, it is going to fall inside it.






          share|cite|improve this answer









          $endgroup$












          • $begingroup$
            this is within the classical electromagnetic interactions , fair enough, but one should not call them photons. Photons have to be treated quantum mechanically. and it propagates the false, imo, intuition that a photon can be partly in or out of the horizon. Individual particles are either in and absorbed, or out. It is the probability of this that can be calculated for individual photons. They do build up the electromagnetic wave, in QFT, but still they are individual measureable particles. The wave function of the photon is a wavefunction that builds a probability distribution, not space one
            $endgroup$
            – anna v
            31 mins ago











          • $begingroup$
            See a wavefunction of a photon here cds.cern.ch/record/944002?ln=en .
            $endgroup$
            – anna v
            27 mins ago


















          4












          $begingroup$

          You are thinking of the photon as an extended classical wave, which is not correct within the standard model of particle physics. This is not correct. Photons are point like quantum mechanical particles, and quantum mechanics is all about probabilities.



          A photon approaching a black hole will have a calculable probability to fall through and be captured, or join the photon sphere. This means that a distribution of photons with the same energy and boundary conditions has to be accumulated in order to check the calculation.






          share|cite|improve this answer









          $endgroup$













            Your Answer








            StackExchange.ready(function()
            var channelOptions =
            tags: "".split(" "),
            id: "151"
            ;
            initTagRenderer("".split(" "), "".split(" "), channelOptions);

            StackExchange.using("externalEditor", function()
            // Have to fire editor after snippets, if snippets enabled
            if (StackExchange.settings.snippets.snippetsEnabled)
            StackExchange.using("snippets", function()
            createEditor();
            );

            else
            createEditor();

            );

            function createEditor()
            StackExchange.prepareEditor(
            heartbeatType: 'answer',
            autoActivateHeartbeat: false,
            convertImagesToLinks: false,
            noModals: true,
            showLowRepImageUploadWarning: true,
            reputationToPostImages: null,
            bindNavPrevention: true,
            postfix: "",
            imageUploader:
            brandingHtml: "Powered by u003ca class="icon-imgur-white" href="https://imgur.com/"u003eu003c/au003e",
            contentPolicyHtml: "User contributions licensed under u003ca href="https://creativecommons.org/licenses/by-sa/3.0/"u003ecc by-sa 3.0 with attribution requiredu003c/au003e u003ca href="https://stackoverflow.com/legal/content-policy"u003e(content policy)u003c/au003e",
            allowUrls: true
            ,
            noCode: true, onDemand: true,
            discardSelector: ".discard-answer"
            ,immediatelyShowMarkdownHelp:true
            );



            );













            draft saved

            draft discarded


















            StackExchange.ready(
            function ()
            StackExchange.openid.initPostLogin('.new-post-login', 'https%3a%2f%2fphysics.stackexchange.com%2fquestions%2f475903%2fhow-much-of-a-wave-function-must-reside-inside-event-horizon-for-it-to-be-consum%23new-answer', 'question_page');

            );

            Post as a guest















            Required, but never shown

























            2 Answers
            2






            active

            oldest

            votes








            2 Answers
            2






            active

            oldest

            votes









            active

            oldest

            votes






            active

            oldest

            votes









            5












            $begingroup$

            Introduction



            First of all we need to establish what the question even means (I will restrict all formulas to non-rotating Schwarzschild black holes of mass $M$ for concreteness). There are no bound states of the electromagnetic field near a black hole, even quasi-stationary states of finite wavelength near the photon radius $r = 3GM/c^2$ will decay, a part falling into the black hole, a part to infinity.



            So the question really is about scattering. It turns out that scattering of electromagnetic waves behaves differently based on wavelength. In SI units the wavelength is $lambda = c/(2pi omega)$ and this is also the localization of the photon. For intuition we can picture the photon as a wavepacket localized in a sphere of radius $lambda$. On the other hand, the typical length of the gravitational background is $GM/c^2$. The main parameter that controls the behavior of the scattering is thus the ratio of these lengths $GM/c^2/(c/(2pi omega))$. I will now switch to geometrized $G=c=1$ units and drop a $2pi$ factor, and then the ratio of the wavelength to the size of the black hole is $sim Momega$.




            Large wavelengths



            For $Momega to 0$ the wavelength is much larger than the black hole, "a very small part of the photon is in the black hole". In this limit it can be computed that the total cross-section of an incoming monochromatic, asymptotically planar wave is
            $$sigma = left[4 pi (2 M)^2 right]frac43M^2 omega^2 + mathcalO(omega^3)$$
            It is difficult to interpret the leading-order term as some kind of "overlapping volume" of the wave and the black hole, since that would scale as $M^3omega^3$. However, a sphere of radius $R$ will scatter particles with a cross-section $4 pi R^2$. Taking a wave-packet with a centroid that would be classically absorbed by a rigid sphere of radius $2M$, the factor $4 M^2 omega^2/3$ can be loosely understood as the probability it will actually be absorbed. Quite interestingly, the low-energy photon sees the black hole as a two-dimensional surface interacting with its wave-front rather than a three-dimensional volume.




            Shorter wavelengths



            However, this all changes with increasing frequency/decreasing wavelength. The intermediate regime is impossible to compute analytically, so I just put a plot from Crispino et al. (2007) here (I also recommend the paper for further references):
            enter image description here
            In the plot, $sigma_E^(omega = 0)$ is the low-frequency limit given above, $sigma_E$ is the total cross-section of monochromatic electromagnetic waves (computed numerically), $sigma_S$ is the same for massless scalar waves, and $sigma_O$ is the optical limit which you get from considering photons as point particles
            $$sigma_O = 27 pi M^2$$
            It is now easy to see that once the size of the wavepacket is comparable or smaller than the black hole, you can simply use the following approximate intuition: If the wavepacket centroid is within the photon sphere, it is going to fall inside it.






            share|cite|improve this answer









            $endgroup$












            • $begingroup$
              this is within the classical electromagnetic interactions , fair enough, but one should not call them photons. Photons have to be treated quantum mechanically. and it propagates the false, imo, intuition that a photon can be partly in or out of the horizon. Individual particles are either in and absorbed, or out. It is the probability of this that can be calculated for individual photons. They do build up the electromagnetic wave, in QFT, but still they are individual measureable particles. The wave function of the photon is a wavefunction that builds a probability distribution, not space one
              $endgroup$
              – anna v
              31 mins ago











            • $begingroup$
              See a wavefunction of a photon here cds.cern.ch/record/944002?ln=en .
              $endgroup$
              – anna v
              27 mins ago















            5












            $begingroup$

            Introduction



            First of all we need to establish what the question even means (I will restrict all formulas to non-rotating Schwarzschild black holes of mass $M$ for concreteness). There are no bound states of the electromagnetic field near a black hole, even quasi-stationary states of finite wavelength near the photon radius $r = 3GM/c^2$ will decay, a part falling into the black hole, a part to infinity.



            So the question really is about scattering. It turns out that scattering of electromagnetic waves behaves differently based on wavelength. In SI units the wavelength is $lambda = c/(2pi omega)$ and this is also the localization of the photon. For intuition we can picture the photon as a wavepacket localized in a sphere of radius $lambda$. On the other hand, the typical length of the gravitational background is $GM/c^2$. The main parameter that controls the behavior of the scattering is thus the ratio of these lengths $GM/c^2/(c/(2pi omega))$. I will now switch to geometrized $G=c=1$ units and drop a $2pi$ factor, and then the ratio of the wavelength to the size of the black hole is $sim Momega$.




            Large wavelengths



            For $Momega to 0$ the wavelength is much larger than the black hole, "a very small part of the photon is in the black hole". In this limit it can be computed that the total cross-section of an incoming monochromatic, asymptotically planar wave is
            $$sigma = left[4 pi (2 M)^2 right]frac43M^2 omega^2 + mathcalO(omega^3)$$
            It is difficult to interpret the leading-order term as some kind of "overlapping volume" of the wave and the black hole, since that would scale as $M^3omega^3$. However, a sphere of radius $R$ will scatter particles with a cross-section $4 pi R^2$. Taking a wave-packet with a centroid that would be classically absorbed by a rigid sphere of radius $2M$, the factor $4 M^2 omega^2/3$ can be loosely understood as the probability it will actually be absorbed. Quite interestingly, the low-energy photon sees the black hole as a two-dimensional surface interacting with its wave-front rather than a three-dimensional volume.




            Shorter wavelengths



            However, this all changes with increasing frequency/decreasing wavelength. The intermediate regime is impossible to compute analytically, so I just put a plot from Crispino et al. (2007) here (I also recommend the paper for further references):
            enter image description here
            In the plot, $sigma_E^(omega = 0)$ is the low-frequency limit given above, $sigma_E$ is the total cross-section of monochromatic electromagnetic waves (computed numerically), $sigma_S$ is the same for massless scalar waves, and $sigma_O$ is the optical limit which you get from considering photons as point particles
            $$sigma_O = 27 pi M^2$$
            It is now easy to see that once the size of the wavepacket is comparable or smaller than the black hole, you can simply use the following approximate intuition: If the wavepacket centroid is within the photon sphere, it is going to fall inside it.






            share|cite|improve this answer









            $endgroup$












            • $begingroup$
              this is within the classical electromagnetic interactions , fair enough, but one should not call them photons. Photons have to be treated quantum mechanically. and it propagates the false, imo, intuition that a photon can be partly in or out of the horizon. Individual particles are either in and absorbed, or out. It is the probability of this that can be calculated for individual photons. They do build up the electromagnetic wave, in QFT, but still they are individual measureable particles. The wave function of the photon is a wavefunction that builds a probability distribution, not space one
              $endgroup$
              – anna v
              31 mins ago











            • $begingroup$
              See a wavefunction of a photon here cds.cern.ch/record/944002?ln=en .
              $endgroup$
              – anna v
              27 mins ago













            5












            5








            5





            $begingroup$

            Introduction



            First of all we need to establish what the question even means (I will restrict all formulas to non-rotating Schwarzschild black holes of mass $M$ for concreteness). There are no bound states of the electromagnetic field near a black hole, even quasi-stationary states of finite wavelength near the photon radius $r = 3GM/c^2$ will decay, a part falling into the black hole, a part to infinity.



            So the question really is about scattering. It turns out that scattering of electromagnetic waves behaves differently based on wavelength. In SI units the wavelength is $lambda = c/(2pi omega)$ and this is also the localization of the photon. For intuition we can picture the photon as a wavepacket localized in a sphere of radius $lambda$. On the other hand, the typical length of the gravitational background is $GM/c^2$. The main parameter that controls the behavior of the scattering is thus the ratio of these lengths $GM/c^2/(c/(2pi omega))$. I will now switch to geometrized $G=c=1$ units and drop a $2pi$ factor, and then the ratio of the wavelength to the size of the black hole is $sim Momega$.




            Large wavelengths



            For $Momega to 0$ the wavelength is much larger than the black hole, "a very small part of the photon is in the black hole". In this limit it can be computed that the total cross-section of an incoming monochromatic, asymptotically planar wave is
            $$sigma = left[4 pi (2 M)^2 right]frac43M^2 omega^2 + mathcalO(omega^3)$$
            It is difficult to interpret the leading-order term as some kind of "overlapping volume" of the wave and the black hole, since that would scale as $M^3omega^3$. However, a sphere of radius $R$ will scatter particles with a cross-section $4 pi R^2$. Taking a wave-packet with a centroid that would be classically absorbed by a rigid sphere of radius $2M$, the factor $4 M^2 omega^2/3$ can be loosely understood as the probability it will actually be absorbed. Quite interestingly, the low-energy photon sees the black hole as a two-dimensional surface interacting with its wave-front rather than a three-dimensional volume.




            Shorter wavelengths



            However, this all changes with increasing frequency/decreasing wavelength. The intermediate regime is impossible to compute analytically, so I just put a plot from Crispino et al. (2007) here (I also recommend the paper for further references):
            enter image description here
            In the plot, $sigma_E^(omega = 0)$ is the low-frequency limit given above, $sigma_E$ is the total cross-section of monochromatic electromagnetic waves (computed numerically), $sigma_S$ is the same for massless scalar waves, and $sigma_O$ is the optical limit which you get from considering photons as point particles
            $$sigma_O = 27 pi M^2$$
            It is now easy to see that once the size of the wavepacket is comparable or smaller than the black hole, you can simply use the following approximate intuition: If the wavepacket centroid is within the photon sphere, it is going to fall inside it.






            share|cite|improve this answer









            $endgroup$



            Introduction



            First of all we need to establish what the question even means (I will restrict all formulas to non-rotating Schwarzschild black holes of mass $M$ for concreteness). There are no bound states of the electromagnetic field near a black hole, even quasi-stationary states of finite wavelength near the photon radius $r = 3GM/c^2$ will decay, a part falling into the black hole, a part to infinity.



            So the question really is about scattering. It turns out that scattering of electromagnetic waves behaves differently based on wavelength. In SI units the wavelength is $lambda = c/(2pi omega)$ and this is also the localization of the photon. For intuition we can picture the photon as a wavepacket localized in a sphere of radius $lambda$. On the other hand, the typical length of the gravitational background is $GM/c^2$. The main parameter that controls the behavior of the scattering is thus the ratio of these lengths $GM/c^2/(c/(2pi omega))$. I will now switch to geometrized $G=c=1$ units and drop a $2pi$ factor, and then the ratio of the wavelength to the size of the black hole is $sim Momega$.




            Large wavelengths



            For $Momega to 0$ the wavelength is much larger than the black hole, "a very small part of the photon is in the black hole". In this limit it can be computed that the total cross-section of an incoming monochromatic, asymptotically planar wave is
            $$sigma = left[4 pi (2 M)^2 right]frac43M^2 omega^2 + mathcalO(omega^3)$$
            It is difficult to interpret the leading-order term as some kind of "overlapping volume" of the wave and the black hole, since that would scale as $M^3omega^3$. However, a sphere of radius $R$ will scatter particles with a cross-section $4 pi R^2$. Taking a wave-packet with a centroid that would be classically absorbed by a rigid sphere of radius $2M$, the factor $4 M^2 omega^2/3$ can be loosely understood as the probability it will actually be absorbed. Quite interestingly, the low-energy photon sees the black hole as a two-dimensional surface interacting with its wave-front rather than a three-dimensional volume.




            Shorter wavelengths



            However, this all changes with increasing frequency/decreasing wavelength. The intermediate regime is impossible to compute analytically, so I just put a plot from Crispino et al. (2007) here (I also recommend the paper for further references):
            enter image description here
            In the plot, $sigma_E^(omega = 0)$ is the low-frequency limit given above, $sigma_E$ is the total cross-section of monochromatic electromagnetic waves (computed numerically), $sigma_S$ is the same for massless scalar waves, and $sigma_O$ is the optical limit which you get from considering photons as point particles
            $$sigma_O = 27 pi M^2$$
            It is now easy to see that once the size of the wavepacket is comparable or smaller than the black hole, you can simply use the following approximate intuition: If the wavepacket centroid is within the photon sphere, it is going to fall inside it.







            share|cite|improve this answer












            share|cite|improve this answer



            share|cite|improve this answer










            answered 1 hour ago









            VoidVoid

            11.4k11959




            11.4k11959











            • $begingroup$
              this is within the classical electromagnetic interactions , fair enough, but one should not call them photons. Photons have to be treated quantum mechanically. and it propagates the false, imo, intuition that a photon can be partly in or out of the horizon. Individual particles are either in and absorbed, or out. It is the probability of this that can be calculated for individual photons. They do build up the electromagnetic wave, in QFT, but still they are individual measureable particles. The wave function of the photon is a wavefunction that builds a probability distribution, not space one
              $endgroup$
              – anna v
              31 mins ago











            • $begingroup$
              See a wavefunction of a photon here cds.cern.ch/record/944002?ln=en .
              $endgroup$
              – anna v
              27 mins ago
















            • $begingroup$
              this is within the classical electromagnetic interactions , fair enough, but one should not call them photons. Photons have to be treated quantum mechanically. and it propagates the false, imo, intuition that a photon can be partly in or out of the horizon. Individual particles are either in and absorbed, or out. It is the probability of this that can be calculated for individual photons. They do build up the electromagnetic wave, in QFT, but still they are individual measureable particles. The wave function of the photon is a wavefunction that builds a probability distribution, not space one
              $endgroup$
              – anna v
              31 mins ago











            • $begingroup$
              See a wavefunction of a photon here cds.cern.ch/record/944002?ln=en .
              $endgroup$
              – anna v
              27 mins ago















            $begingroup$
            this is within the classical electromagnetic interactions , fair enough, but one should not call them photons. Photons have to be treated quantum mechanically. and it propagates the false, imo, intuition that a photon can be partly in or out of the horizon. Individual particles are either in and absorbed, or out. It is the probability of this that can be calculated for individual photons. They do build up the electromagnetic wave, in QFT, but still they are individual measureable particles. The wave function of the photon is a wavefunction that builds a probability distribution, not space one
            $endgroup$
            – anna v
            31 mins ago





            $begingroup$
            this is within the classical electromagnetic interactions , fair enough, but one should not call them photons. Photons have to be treated quantum mechanically. and it propagates the false, imo, intuition that a photon can be partly in or out of the horizon. Individual particles are either in and absorbed, or out. It is the probability of this that can be calculated for individual photons. They do build up the electromagnetic wave, in QFT, but still they are individual measureable particles. The wave function of the photon is a wavefunction that builds a probability distribution, not space one
            $endgroup$
            – anna v
            31 mins ago













            $begingroup$
            See a wavefunction of a photon here cds.cern.ch/record/944002?ln=en .
            $endgroup$
            – anna v
            27 mins ago




            $begingroup$
            See a wavefunction of a photon here cds.cern.ch/record/944002?ln=en .
            $endgroup$
            – anna v
            27 mins ago











            4












            $begingroup$

            You are thinking of the photon as an extended classical wave, which is not correct within the standard model of particle physics. This is not correct. Photons are point like quantum mechanical particles, and quantum mechanics is all about probabilities.



            A photon approaching a black hole will have a calculable probability to fall through and be captured, or join the photon sphere. This means that a distribution of photons with the same energy and boundary conditions has to be accumulated in order to check the calculation.






            share|cite|improve this answer









            $endgroup$

















              4












              $begingroup$

              You are thinking of the photon as an extended classical wave, which is not correct within the standard model of particle physics. This is not correct. Photons are point like quantum mechanical particles, and quantum mechanics is all about probabilities.



              A photon approaching a black hole will have a calculable probability to fall through and be captured, or join the photon sphere. This means that a distribution of photons with the same energy and boundary conditions has to be accumulated in order to check the calculation.






              share|cite|improve this answer









              $endgroup$















                4












                4








                4





                $begingroup$

                You are thinking of the photon as an extended classical wave, which is not correct within the standard model of particle physics. This is not correct. Photons are point like quantum mechanical particles, and quantum mechanics is all about probabilities.



                A photon approaching a black hole will have a calculable probability to fall through and be captured, or join the photon sphere. This means that a distribution of photons with the same energy and boundary conditions has to be accumulated in order to check the calculation.






                share|cite|improve this answer









                $endgroup$



                You are thinking of the photon as an extended classical wave, which is not correct within the standard model of particle physics. This is not correct. Photons are point like quantum mechanical particles, and quantum mechanics is all about probabilities.



                A photon approaching a black hole will have a calculable probability to fall through and be captured, or join the photon sphere. This means that a distribution of photons with the same energy and boundary conditions has to be accumulated in order to check the calculation.







                share|cite|improve this answer












                share|cite|improve this answer



                share|cite|improve this answer










                answered 3 hours ago









                anna vanna v

                163k8154459




                163k8154459



























                    draft saved

                    draft discarded
















































                    Thanks for contributing an answer to Physics Stack Exchange!


                    • Please be sure to answer the question. Provide details and share your research!

                    But avoid


                    • Asking for help, clarification, or responding to other answers.

                    • Making statements based on opinion; back them up with references or personal experience.

                    Use MathJax to format equations. MathJax reference.


                    To learn more, see our tips on writing great answers.




                    draft saved


                    draft discarded














                    StackExchange.ready(
                    function ()
                    StackExchange.openid.initPostLogin('.new-post-login', 'https%3a%2f%2fphysics.stackexchange.com%2fquestions%2f475903%2fhow-much-of-a-wave-function-must-reside-inside-event-horizon-for-it-to-be-consum%23new-answer', 'question_page');

                    );

                    Post as a guest















                    Required, but never shown





















































                    Required, but never shown














                    Required, but never shown












                    Required, but never shown







                    Required, but never shown

































                    Required, but never shown














                    Required, but never shown












                    Required, but never shown







                    Required, but never shown







                    Popular posts from this blog

                    Oświęcim Innehåll Historia | Källor | Externa länkar | Navigeringsmeny50°2′18″N 19°13′17″Ö / 50.03833°N 19.22139°Ö / 50.03833; 19.2213950°2′18″N 19°13′17″Ö / 50.03833°N 19.22139°Ö / 50.03833; 19.221393089658Nordisk familjebok, AuschwitzInsidan tro och existensJewish Community i OświęcimAuschwitz Jewish Center: MuseumAuschwitz Jewish Center

                    Valle di Casies Indice Geografia fisica | Origini del nome | Storia | Società | Amministrazione | Sport | Note | Bibliografia | Voci correlate | Altri progetti | Collegamenti esterni | Menu di navigazione46°46′N 12°11′E / 46.766667°N 12.183333°E46.766667; 12.183333 (Valle di Casies)46°46′N 12°11′E / 46.766667°N 12.183333°E46.766667; 12.183333 (Valle di Casies)Sito istituzionaleAstat Censimento della popolazione 2011 - Determinazione della consistenza dei tre gruppi linguistici della Provincia Autonoma di Bolzano-Alto Adige - giugno 2012Numeri e fattiValle di CasiesDato IstatTabella dei gradi/giorno dei Comuni italiani raggruppati per Regione e Provincia26 agosto 1993, n. 412Heraldry of the World: GsiesStatistiche I.StatValCasies.comWikimedia CommonsWikimedia CommonsValle di CasiesSito ufficialeValle di CasiesMM14870458910042978-6

                    Typsetting diagram chases (with TikZ?) Announcing the arrival of Valued Associate #679: Cesar Manara Planned maintenance scheduled April 17/18, 2019 at 00:00UTC (8:00pm US/Eastern)How to define the default vertical distance between nodes?Draw edge on arcNumerical conditional within tikz keys?TikZ: Drawing an arc from an intersection to an intersectionDrawing rectilinear curves in Tikz, aka an Etch-a-Sketch drawingLine up nested tikz enviroments or how to get rid of themHow to place nodes in an absolute coordinate system in tikzCommutative diagram with curve connecting between nodesTikz with standalone: pinning tikz coordinates to page cmDrawing a Decision Diagram with Tikz and layout manager