1 / 113

Benvenuti al Mera-TeV!

Benvenuti al Mera-TeV!. 4-5-6 Ottobre 2011 Sala “POE” di OAB a Merate. Lorenzo Sironi. FATE DOMANDE!. Le domande sono gradite, anche prima della fine dei contributi.

rinah-hicks
Download Presentation

Benvenuti al Mera-TeV!

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Benvenuti al Mera-TeV! 4-5-6 Ottobre 2011 Sala “POE” di OAB a Merate

  2. Lorenzo Sironi

  3. FATE DOMANDE! • Le domande sono gradite, anche prima della fine dei contributi. • L'incontro è volutamente informale, e lo spirito è orientato alla comprensione delle tematiche ed alla interazione tra i partecipanti.

  4. SOCIAL EVENT w Visita alle Cupole Zeiss e Ruths: Mercoledì 5, ore 18.15

  5. SOCIAL DINNER • Taverna dei Cacciatori – Imbersago • Ore 20.00 Mercoledì • Partenza da Osservatorio ore 19.45

  6. Pranzi e Pause Caffè • Pranzi: alle 13.00 nel parco, di fronte alla Cupola Ruths • Coffe Breaks: nella Biblioteca, piano seminterrato edificio principale.

  7. Buon Mera-TeV!!

  8. Beaming

  9. Radio-loud AGNs Gamma Ray Bursts ~ 10-5 Mo in a few sec G~300 ~ 0.1 Mo yr-1 G~20

  10. Text book special relativity Lorentz transformations: v along x x’ = G (x – vt) y’ = y z’ = z t’ = G (t – v x/c2) x = G (x’ + vt’) y = y’ z = z’ t = G (t’ + v x’/c2) for Dt = 0Dx = Dx’/GContraction for Dx’ = 0Dt = G Dt’time dilation To remember: mesons created at a height of ~15 km can reach the earth, even if their lifetime is a few microsec  ct’life=hundreds of meters.

  11. Can we see contracted spheres? v=0 G=1 v v=0.866c G=2 Einstein: Yes!

  12. v=0 G=1 James Terrel 1959 NO! Rotation, not contraction! Roger Penrose 1959 v v=0.866c G=2

  13. Relativity with photons From rulers and clocks to photographs and frequencies Or: from elementary particles to extended objects

  14. The moving square b=0 b=0.5 Your camera, very far away

  15. The moving square ltot = l’ (b+1/G) max:21/2l’ (diag) min: l’ (for b=0) t=l’/c l’/G vt=bl’

  16. l’cosa= bl’  cosa = b cos(p-p/2-a) = sina = 1/G l’ p/2-a

  17. a ) p/2-a

  18. p/2-a

  19. Time Dte = emission time in lab frame Dte’ = emission time in comov. frame Dte = Dte’ G CD = cDte – cDtebcosqDtA= Dte (1-bcosq)  DtA= Dte’ G(1-bcosq)

  20. 1 d = G(1-bcosq) Relativistic Doppler factor d DtA= Dte’ G(1-bcosq) n= n’ / G(1-bcosq) Standard relativity You remain in lab frame You change frame Doppler effect

  21. 1 d= G(1-bcosq) Relativistic Doppler factor d { 2G for q=0oG for q=1/G 1/Gforq=90o = At small angles, Doppler wins over Spec. Relat.

  22. 25 light years in 3 years… the velocity is 8.3 c

  23. v=0.99c Nucleo

  24. Dsapp b sinq vDtesinq bapp = =vapp = DtA 1-bcosq Dte (1-bcosq) There is no G. Correct? q=0o bapp=0 cosq=b; sinq=1/G  bapp=bG q=90obapp=b

  25. Aberration of light

  26. Aberration of light sinq = sinq’/d dW =dW’/d2

  27. Aberration of light v K K’ sinq = sinq’/d dW = dW’/d2

  28. I(n) I’(n’) = invariant = n3 n’3 erg E I(n) = = cm2 s Hz sterad dAdt dn dW Observed vs intrinsic Intensity I(n) = d3I’(n’)

  29. I(n) I’(n’) = invariant = n3 n’3 erg E I(n) = = cm2 s Hz sterad dAdt dn dW Observed vs intrinsic Intensity I(n) = d3I’(n’)

  30. I(n) I’(n’) = invariant = n3 n’3 erg E’d = I(n) = d3I’(n’) = cm2 s Hz sterad dA’dW’/d2 = = I F d4F’ d4I’ Observed vs intrinsic Intensity I(n) = d3I’(n’) dblueshift d time d2 aberration

  31. v=0 L=100 W

  32. v=0.995c G=10 L=0.6mW L=16MW L=10mW

  33. v=0.995c G=10 …….? blazars radiogalaxies

  34. v=0.995c G=10 blazars! blazars radiogalaxies

  35. v counterjet (invisible) jet v

  36. Radiation processes

  37. Line emission and radiative transitions in atoms and molecules • Breemstrahlung/Blackbody • Curvature radiation • Cherenkov • Annihilation • Unruh radiation • Hawking radiation • Synchrotron • Inverse Compton Radiation processes

  38. E V=0

  39. E V(g=2) Contracted sphere… E-field lines at time 9.00 point to… where the charge is at 9.00 Charge at time 9.00 Breaking news: what happens with the gravitational field?

  40. dP = e2a2sin2Q dW 4p c3 Stop at 8:00 V http://www.cco.caltech.edu/~phys1/java/phys1/MovingCharge/MovingCharge.html

  41. dP = e2a2sin2Q dW4p c3 P = 2 e2a2 3c3

  42. Synchrotron

  43. d e (gmv) FL = = v x B c dt Synchrotron • Ingredients: Magnetic field and relativistic charges • Responsible: Lorentz force • Curiously, the Lorentz force doesn’t work. q

  44. Total losses Pe = P’e P=E/t and E and t Lorentz transform in the same way Please, Pe is not Preceived!!

  45. 2e2 2e2 Pe = P’e = a’2 = (a’2 + a’2 ) 3c3 3c3 Total losses

  46. 2e2 2e2 Pe = P’e = a’2 = (a’2 + a’2 ) 3c3 3c3 Total losses a’|| = 0 a’ = g2a 2e2 Pe = P’e= g2 a2 3c3 ev B sinq a = g mc

  47. 2e2 2e2 Pe = P’e = a’2 = (a’2 + a’2 ) 3c3 3c3 2e4 PS(q) = B2g2 b2 sin2q 3m2c3 Total losses a’|| = 0 a’ = g2a 2e2 Pe = P’e= g2 a2 3c3 ev B sinq a = g mc

  48. 2e2 2e2 Pe = P’e = a’2 = (a’2 + a’2 ) 3c3 3c3 2e4 PS(q) = B2g2 b2 sin2q 3m2c3 Total losses a’|| = 0 a’ = g2a 2e2 PS(q) = 2sTcUBg2 b2 sin2q Pe = P’e= g2 a2 3c3 ev B sinq a = g mc

  49. 2e2 2e2 Pe = P’e = a’2 = (a’2 + a’2 ) 3c3 3c3 2e4 PS(q) = B2g2 b2 sin2q 3m2c3 <PS> = 4 sTcUBg2 b2 3 Total losses a’|| = 0 a’ = g2a 2e2 PS(q) = 2sTcUBg2 b2 sin2q Pe = P’e= g2 a2 3c3 ev B sinq a = g mc If pitch angles are isotropic

More Related