ASTR 1040 Recitation: Active Galactic Nucleii
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1 ASTR 1040 Recitation: Active Galactic Nucleii Ryan Orvedahl Department of Astrophysical and Planetary Sciences April 14 & 16, 2014
2 This Week Night Observing: Monday April 14 (8:30 pm) Midterm III: Thursday April 17 (9:30 am) Review Session: Wednesday April 16 (5:00 pm G125) Heliostat Observing: Friday April 18 (2:30-4:30 pm) R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 2 / 19
3 Today s Schedule Past/Current Homework or Lecture Questions? Redshift Quasars Active Galactic Nucleii Faster Then Light Travel? R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 3 / 19
4 Cosmological Redshift The universe is expanding, according to SNe Ia Space expands wavelengths expand Longer λ Redshift 1 + z = λ obs /λ 0 R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 4 / 19
5 Cosmological Redshift R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 5 / 19
6 How Do We Observe Cosmological Redshift? λ obs 1 + z = λ obs /λ 0 d = v/h 0 cz/h 0 R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 6 / 19
7 Active Galactic Nucleii 1960s: observes newly discovered radio sources with visible light Typically look like normal galaxies 3C 273: looks like blue star, strong emission lines that did not seem to correspond to any known element After a few months, H emission at z 0.17 Maarten Schmidt R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 7 / 19
8 AGN & Quasars Luminosity of 3C 273: L = W L L MW R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 8 / 19
9 AGN & Quasars Luminosity of 3C 273: L = W L L MW Soon find many more objects with even larger redshifts R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 8 / 19
10 AGN & Quasars Luminosity of 3C 273: L = W L L MW Soon find many more objects with even larger redshifts First few objects were strong radio sources and look like stars in visible light R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 8 / 19
11 AGN & Quasars Luminosity of 3C 273: L = W L L MW Soon find many more objects with even larger redshifts First few objects were strong radio sources and look like stars in visible light Given name Quasars: QUAsi-StellAr Radio Sources R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 8 / 19
12 What Powers A Quasar? Part I How massive are they? Luminosity tells us how much mass they accrete how? R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 9 / 19
13 What Powers A Quasar? Part I How massive are they? Luminosity tells us how much mass they accrete how? L = Mc 2 R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 9 / 19
14 What Powers A Quasar? Part I How massive are they? Luminosity tells us how much mass they accrete how? L = Mc 2 Observed L gives M 1 M /yr R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 9 / 19
15 What Powers A Quasar? Part I How massive are they? Luminosity tells us how much mass they accrete how? L = Mc 2 Observed L gives M 1 M /yr Of all galaxies we observe, only 1% are active R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & 16 9 / 19
16 What Powers A Quasar? Part I Only 1% of galaxies are active 2 possibilities R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
17 What Powers A Quasar? Part I Only 1% of galaxies are active 2 possibilities 1 All galaxies are active for 1% of their life t life 1% t universe 10 8 yrs R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
18 What Powers A Quasar? Part I Only 1% of galaxies are active 2 possibilities 1 All galaxies are active for 1% of their life t life 1% t universe 10 8 yrs 2 Only 1% of galaxies are active for 100% of their life t life 100% t universe yrs R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
19 What Powers A Quasar? Part I How massive are they? R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
20 What Powers A Quasar? Part I How massive are they? We just estimated their lifetime, t life R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
21 What Powers A Quasar? Part I How massive are they? We just estimated their lifetime, t life We measure L, which gives us M 1 M / yr R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
22 What Powers A Quasar? Part I How massive are they? We just estimated their lifetime, t life We measure L, which gives us M 1 M / yr Can estimate their mass: M R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
23 What Powers A Quasar? Part II What about their size? R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
24 What Powers A Quasar? Part II What about their size? Look at surface blemishes Fastest possible variation gives a time scale Turn the time scale into a distance scale through propagation speed R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
25 What Powers A Quasar? Part II What about their size? Pretty short timescales: seconds - hours Gives size of a few light-minutes to light-hours Distance from Sun to Earth is 8 light-minutes Distance from Sun to Saturn is 45 light-minutes Distance from Sun to Pluto is 5.5 light-hours Black Hole!! R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
26 Quasar Characteristics R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
27 Quasar Characteristics Jets Broad Line Region Narrow Line Region Obscuring Torus R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
28 Why Does It Have Jets? Accretion disc is very hot, mainly plasma Magnetic field becomes trapped in plasma (Frozen-In) Field becomes wrapped around rotation axis R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
29 Frozen-In Condition R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
30 Superluminal Jets?? Measure jet on sky (use VLBI for best resolution) Wait some time, measure it again Spatial & time difference give speeds of 6c?? R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
31 Superluminal Jets Explained R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
32 Superluminal Jets Explained We measure β T v T c = β sin θ 1 β cos θ β max T = βγ > 1 R. Orvedahl (CU Boulder) AGN & Quasars Apr 14 & / 19
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