Sinxrotron nurlanishi

Sinxrotron nurlanishi relyativistik zaryadlangan zarralar tezligiga perpendikulyar tezlanishga ( $a ⊥ v$ ) ta'sir qilganda chiqariladigan elektromagnit nurlanishdir . U sun'iy ravishda zarracha tezlatgichlarining ayrim turlarida yoki tabiiy ravishda magnit maydonlar bo'ylab harakatlanadigan tez elektronlar tomonidan ishlab chiqariladi. Shu tarzda ishlab chiqarilgan radiatsiya xarakterli polarizasyona ega va hosil bo'lgan chastotalar elektromagnit spektrning katta qismida o'zgarishi mumkin.^[1] Sinxrotron nurlanish mexanizmi astrofizikada ko’p uchraydigan effekt hisoblanadi. Ular sharoit bo’lgan hamma joyda uchraydi. Masalan: relyativistik elektronlar va magnit maydoni bo’lgan joylarda. Sinõrotron nurlanish tarqatuvchi asosiy astrofizik obúektlar qatoriga quyidagilar kiradi: relyativistik elektronlar buluti, quyoshning aktiv sohasidan chiqqan nurlar (IV va V tipdagi chaqnashlar), gigant-planetalarning magnitosferalari, galaktik disk (dециmetrli va millimetrli to’lqinda), o’ta yangi yulduzlarni chaqnashdan keyingi qoldiqlari, pulüsarlar, normal galaktikalar, radiogalaktikalar va kvazarlar

Sinxrotron nurlanishi bremsstrahlung nurlanishiga o'xshaydi, bu tezlanish harakat yo'nalishiga parallel bo'lganda zaryadlangan zarracha tomonidan chiqariladi. Magnit maydondagi zarrachalar chiqaradigan nurlanishning umumiy atamasi giromagnit nurlanishdir, buning uchun sinxrotron nurlanishi ultra relyativistik maxsus jarayon. Magnit maydonda nisbiy bo'lmagan harakatlanuvchi zaryadlangan zarralar tomonidan chiqariladigan radiatsiya siklotron emissiyasi deb ataladi.^[2] Yengil relyativistik diapazondagi zarralar uchun (yorug'lik tezligining ≈85%) emissiya girosinxrotron nurlanishi deb ataladi.^[3]

Astrofizikada sinxrotron emissiyasi, masalan, qora tuynuk atrofida zaryadlangan zarrachaning ultra relyativistik harakati tufayli sodir bo'ladi.^[4] Qora tuynuk atrofida aylana geodeziyani kuzatib borganida, sinxrotron nurlanishi harakat ultra relyativistik rejimda bo'lgan fotosferaga yaqin orbitalar uchun sodir bo'ladi.

Tarixi[tahrir | manbasini tahrirlash]

Sinxrotron nurlanishi birinchi marta texnik Floyd Xaber tomonidan 1947-yil 24-aprelda Nyu-Yorkning Shenektadi shahridagi General Electric tadqiqot laboratoriyasining 70 MeV elektron sinxrotronida kuzatilgan.^[5] Bu birinchi qurilgan sinxrotron bo'lmasa-da, u radiatsiyani bevosita kuzatish imkonini beruvchi shaffof vakuum trubkasi bilan birinchi bo'ldi.^[6]

Gerbert Pollok aytganidek:^[7]

On April 24, Langmuir and I were running the machine and as usual were trying to push the electron gun and its associated pulse transformer to the limit. Some intermittent sparking had occurred and we asked the technician to observe with a mirror around the protective concrete wall. He immediately signaled to turn off the synchrotron as "he saw an arc in the tube". The vacuum was still excellent, so Langmuir and I came to the end of the wall and observed. At first we thought it might be due to Cherenkov radiation, but it soon became clearer that we were seeing Ivanenko and Pomeranchuk radiation.^[8]

Tavsif[tahrir | manbasini tahrirlash]

Maksvell tenglamalarining bevosita natijasi shundaki, tezlashtirilgan zaryadlangan zarralar doimo elektromagnit nurlanish chiqaradi. Sinxrotron nurlanishi - relativistik tezlikda harakatlanadigan zaryadlangan zarrachalarning harakat yo'nalishiga perpendikulyar tezlanishga ega bo'lgan maxsus holat, odatda magnit maydonda. Bunday maydonda maydondan kelib chiqadigan kuch har doim ham harakat yo'nalishiga, ham maydon yo'nalishiga perpendikulyar bo'ladi, bu Lorents kuch qonunida ko'rsatilgan.

Radiatsiya tomonidan olib boriladigan quvvat ( SI birliklarida ) relativistik Larmor formulasi bilan topiladi:^[9]

P_{\gamma }={\frac {1}{6\pi \varepsilon _{0}}}{\frac {q^{2}a^{2}}{c^{3}}}\gamma ^{4},

Sinxrotron nurlanishi astronomik ob'ektlar tomonidan ham hosil bo'ladi, odatda relyativistik elektronlar magnit maydonlar orqali spiral (va shuning uchun tezlikni o'zgartiradi). Uning ikkita xarakteristikasiga energiya qonuni energiya spektrlari va qutblanish kiradi.^[10] Bu relyativistik zaryadlangan zarrachalar mavjud bo'lgan joyda quyoshdan tashqari magnit maydonlarni o'rganishda eng kuchli vositalardan biri hisoblanadi. Ko'pgina ma'lum kosmik radio manbalari sinxrotron nurlanishini chiqaradi. U ko'pincha katta kosmik magnit maydonlarning kuchini baholash, shuningdek, yulduzlararo va galaktikalararo muhit tarkibini tahlil qilish uchun ishlatiladi.^[11]

$\varepsilon _{0}$ vakuum o'tkazuvchanligi ,
$q$ zarracha zaryadidir,
$a$ tezlanishning kattaligi,
$c$ yorug'lik tezligi,
$\gamma$ Lorents omilidir .

Tezlatgichlardan sinxrotron nurlanishi[tahrir | manbasini tahrirlash]

Doiraviy tezlatgichlar har doim giromagnit nurlanish hosil qiladi, chunki zarralar magnit maydonda burilib ketadi. Biroq, nurlanishning miqdori va xususiyatlari sodir bo'layotgan tezlanishning tabiatiga juda bog'liq. Masalan, massa farqi tufayli, omil $\gamma ^{4}$ chiqarilgan quvvat formulasida elektronlar proton tezligidan taxminan 10 ¹³ marta energiya chiqaradi degan ma'noni anglatadi.^[12]

Dumaloq tezlatgichlarda sinxrotron nurlanishidan energiya yo‘qotilishi dastlab noqulaylik hisoblangan, chunki yo‘qotishlarni qoplash uchun nurga qo‘shimcha energiya berilishi kerak. Biroq, 1980-yillardan boshlab, tadqiqot uchun ataylab sinxrotron nurlanishining intensiv nurlarini ishlab chiqarish uchun yorug'lik manbalari deb nomlanuvchi dumaloq elektron tezlatgichlar qurilgan.^[13]

Astronomiyada sinxrotron nurlanishi[tahrir | manbasini tahrirlash]

Sinxrotron nurlanishi astronomik ob'ektlar tomonidan ham hosil bo'ladi, odatda relyativistik elektronlar magnit maydonlar orqali spiral (va shuning uchun tezlikni o'zgartiradi). Uning ikkita xarakteristikasiga energiya qonuni energiya spektrlari va qutblanish kiradi.^[10] Bu relyativistik zaryadlangan zarrachalar mavjud bo'lgan joyda quyoshdan tashqari magnit maydonlarni o'rganishda eng kuchli vositalardan biri hisoblanadi. Ko'pgina ma'lum kosmik radio manbalari sinxrotron nurlanishini chiqaradi. U ko'pincha katta kosmik magnit maydonlarning kuchini baholash, shuningdek, yulduzlararo va galaktikalararo muhit tarkibini tahlil qilish uchun ishlatiladi.^[11]

Qo'shimcha ma'lumotlar[tahrir | manbasini tahrirlash]

Bremsstrahlung – Electromagnetic radiation due to deceleration of charged particles
Cyclotron turnover
Free-electron laser – Light source producing extremely brilliant and short pulses of radiation
Radiation reaction – recoil force on an accelerating charged particle caused by the particle emitting electromagnetic radiationPages displaying wikidata descriptions as a fallback
Relativistic beaming – change in the apparent luminosity of emitting matter that is moving close to the speed of lightPages displaying wikidata descriptions as a fallback
Sokolov–Ternov effect – Physical phenomenon of spin-polarization
Synchrotron function

^[14]

Manba[tahrir | manbasini tahrirlash]

↑ „What is synchrotron radiation?“. NIST (inglizcha). 2010-03-02.
↑ Monreal, Benjamin (Jan 2016). „Single-electron cyclotron radiation“. Physics Today. 69-jild, № 1. 70-bet. Bibcode:2016PhT....69a..70M. doi:10.1063/pt.3.3060.
↑ Chen. „Radiative processes from energetic particles II: Gyromagnetic radiation“. New Jersey Institute of Technology. Qaraldi: 2021-yil 10-dekabr.
↑ Brito, João P. B.; Bernar, Rafael P.; Crispino, Luís C. B. (11 June 2020). „Synchrotron geodesic radiation in Schwarzschild–de Sitter spacetime“. Physical Review D (inglizcha). 101-jild, № 12. 124019-bet. arXiv:2006.08887. Bibcode:2020PhRvD.101l4019B. doi:10.1103/PhysRevD.101.124019. ISSN 2470-0010.
↑ Elder, F. R.; Gurewitsch, A. M.; Langmuir, R. V.; Pollock, H. C. (1 June 1947). „Radiation from Electrons in a Synchrotron“. Physical Review. 71-jild, № 11. American Physical Society. 829–830-bet. Bibcode:1947PhRv...71..829E. doi:10.1103/physrev.71.829.5. ISSN 0031-899X.
↑ Mitchell, Edward; Kuhn, Peter; Garman, Elspeth (May 1999). „Demystifying the synchrotron trip: a first time user's guide“. Structure. 7-jild, № 5. R111–R121-bet. doi:10.1016/s0969-2126(99)80063-x. PMID 10378266.
↑ Pollock, Herbert C. (March 1983). „The discovery of synchrotron radiation“. American Journal of Physics. 51-jild, № 3. 278–280-bet. Bibcode:1983AmJPh..51..278P. doi:10.1119/1.13289.
↑ Iwanenko, D.; Pomeranchuk, I. (1 June 1944). „On the Maximal Energy Attainable in a Betatron“. Physical Review. 65-jild, № 11–12. American Physical Society. 343-bet. Bibcode:1944PhRv...65..343I. doi:10.1103/physrev.65.343. ISSN 0031-899X.
↑ Wilson, E. J. N.. An introduction to particle accelerators. Oxford: Oxford University Press, 2001 — 221–223 bet. ISBN 0-19-850829-8.
↑ ^10,0 ^10,1 Vladimir A. Bordovitsyn, "Synchrotron Radiation in Astrophysics" (1999) Synchrotron Radiation Theory and Its Development, ISBN 981-02-3156-3
↑ ^11,0 ^11,1 Klein, Ulrich. Galactic and intergalactic magnetic fields. Cham, Switzerland & New York: Springer, 2014. ISBN 978-3-319-08942-3. OCLC 894893367.
↑ Conte, Mario. An introduction to the physics of particle accelerators, 2nd, Hackensack, N.J.: World Scientific, 2008 — 166 bet. ISBN 978-981-277-960-1.
↑ „History: Of X-rays and synchrotrons“. lightsources.org (2017-yil 21-sentyabr). Qaraldi: 2021-yil 13-dekabr.
↑ {{cite magazine}}: Empty citation (yordam)

[1] „What is synchrotron radiation?“. NIST (inglizcha). 2010-03-02.

[2] Monreal, Benjamin (Jan 2016). „Single-electron cyclotron radiation“. Physics Today. 69-jild, № 1. 70-bet. Bibcode:2016PhT....69a..70M. doi:10.1063/pt.3.3060.

[3] Chen. „Radiative processes from energetic particles II: Gyromagnetic radiation“. New Jersey Institute of Technology. Qaraldi: 2021-yil 10-dekabr.

[4] Brito, João P. B.; Bernar, Rafael P.; Crispino, Luís C. B. (11 June 2020). „Synchrotron geodesic radiation in Schwarzschild–de Sitter spacetime“. Physical Review D (inglizcha). 101-jild, № 12. 124019-bet. arXiv:2006.08887. Bibcode:2020PhRvD.101l4019B. doi:10.1103/PhysRevD.101.124019. ISSN 2470-0010.

[5] Elder, F. R.; Gurewitsch, A. M.; Langmuir, R. V.; Pollock, H. C. (1 June 1947). „Radiation from Electrons in a Synchrotron“. Physical Review. 71-jild, № 11. American Physical Society. 829–830-bet. Bibcode:1947PhRv...71..829E. doi:10.1103/physrev.71.829.5. ISSN 0031-899X.

[6] Mitchell, Edward; Kuhn, Peter; Garman, Elspeth (May 1999). „Demystifying the synchrotron trip: a first time user's guide“. Structure. 7-jild, № 5. R111–R121-bet. doi:10.1016/s0969-2126(99)80063-x. PMID 10378266.

[7] Pollock, Herbert C. (March 1983). „The discovery of synchrotron radiation“. American Journal of Physics. 51-jild, № 3. 278–280-bet. Bibcode:1983AmJPh..51..278P. doi:10.1119/1.13289.

[8] Iwanenko, D.; Pomeranchuk, I. (1 June 1944). „On the Maximal Energy Attainable in a Betatron“. Physical Review. 65-jild, № 11–12. American Physical Society. 343-bet. Bibcode:1944PhRv...65..343I. doi:10.1103/physrev.65.343. ISSN 0031-899X.

[9] Wilson, E. J. N.. An introduction to particle accelerators. Oxford: Oxford University Press, 2001 — 221–223 bet. ISBN 0-19-850829-8.

[books.google.com-10] 10,0 ^10,1 Vladimir A. Bordovitsyn, "Synchrotron Radiation in Astrophysics" (1999) Synchrotron Radiation Theory and Its Development, ISBN 981-02-3156-3

[Klein_2014-11] 11,0 ^11,1 Klein, Ulrich. Galactic and intergalactic magnetic fields. Cham, Switzerland & New York: Springer, 2014. ISBN 978-3-319-08942-3. OCLC 894893367.

[12] Conte, Mario. An introduction to the physics of particle accelerators, 2nd, Hackensack, N.J.: World Scientific, 2008 — 166 bet. ISBN 978-981-277-960-1.

[13] „History: Of X-rays and synchrotrons“. lightsources.org (2017-yil 21-sentyabr). Qaraldi: 2021-yil 13-dekabr.

[14] {{cite magazine}}: Empty citation (yordam)

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