White Dwarfs and Electron Degeneracy
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1 White Dwarfs and Electron Degeneracy Farley V. Ferrante Southern Methodist University Sirius A and B 1 December 2017 SMU PHYSICS 1
2 Outline Stellar astrophysics White dwarfs Dwarf novae Classical novae Supernovae Neutron stars 1 December 2017 SMU PHYSICS 2
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4 Pogson s ratio: December 2017 SMU PHYSICS 4
5 Distance Modulus m M = 5 log ( ) 10 d 1 Absolute magnitude (M) Apparent magnitude of an object at a standard luminosity distance of exactly 10.0 parsecs (~32.6 ly) from the observer on Earth Allows true luminosity of astronomical objects to be compared without regard to their distances Unit: parsec (pc) Distance at which 1 AU subtends an angle of 1 1 AU = m ( 1.50 x 10 8 km) 1 pc 3.26 ly 1 pc AU 1 December 2017 SMU PHYSICS 5
6 Stellar Astrophysics Stefan-Boltzmann Law: 2π k Fbol = σt = = x ergs cm K 15ch ; σ Effective temperature of a star: Temp. of a black body with the same luminosity per surface area Stars can be treated as black body radiators to a good approximation Effective surface temperature can be obtained from the B-V color index with the Ballesteros equation: T = ( B V) ( B V) Luminosity: * E L= πr σt 1 December 2017 SMU PHYSICS 6
7 H-R Diagram
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10 White dwarf Core of solar mass star Pauli exclusion principle: Electron degeneracy Degenerate Fermi gas of oxygen and carbon 1 teaspoon weigh ~5 tons No energy produced from fusion or gravitational contraction Hot white dwarf NGC The white dwarf is surrounded by a "cocoons" of the gas ejected in the collapse toward the white dwarf stage of stellar evolution. 1 December 2017 SMU PHYSICS 10
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21 Mass/radius relation for degenerate star Stellar mass = M; radius = R Gravitational potential energy: Heisenberg uncertainty: Electron density: Egr x p n 3GM = 5R 3N = 4 π R h 3 2 M m R p 3 x n 1 3 p h x hn 1 3 Kinetic energy: p M M ε = K = Nε = ε m e m p mm e p R 1 December 2017 SMU PHYSICS 21
22 Mass/radius relation for degenerate star Total energy: E = K + U 2 h M 5 m m e 3 p 5 3 R 2 GM R 2 Find R by minimizing E: de dr 2 h M m m e 5 3 p 5 3 R 3 + GM 2 R 2 = 0 Radius decreases as mass increases: 2 M R h 5 Gm e m p December 2017 SMU PHYSICS 22
23 Mass vs radius relation 1 December 2017 SMU PHYSICS 23
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28 Mass vs radius relation 1 December 2017 SMU PHYSICS 28
29 ROTSE Robotic Optical Transient Search Experiment Original purpose: Observe GRB optical counterpart ( afterglow ) Observation & detection of optical transients (seconds to days) Robotic operating system o Automated interacting Linux daemons o Sensitivity to short time-scale variation o Efficient analysis of large data stream o Recognition of rare signals Current research: o GRB response o SNe search (RSVP) o Variable star search o Other transients: AGN, CV (dwarf novae), flare stars, novae, variable stars, X-ray binaries ROTSE-IIIa Australian National Observatory 1 December 2017 SMU PHYSICS 29
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33 ROTSE-I 1 st successful robotic telescope ; Los Alamos, NM Co-mounted, 4-fold telephoto array (Cannon 200 mm lenses) CCD o 2k x 2k Thomson o Thick o Front illuminated o Red sensitive o R-band equivalent o Operated clear (unfiltered) Optics o Aperture (cm): 11.1 o f-ratio: 1.8 o FOV: Sensitivity (magnitude): o Best: 15.7 Slew time (90 ): 2.8 s : Observed 1 st GRB afterglow in progress o Landmark event o Proof of concept 1 December 2017 SMU PHYSICS 33
34 ROTSE-III 2003 present 4 Cassegrain telescopes CCD o o o o o Optics Thin Back illuminated Blue-sensitive High QE (UBVRI bands) Default photometry calibrated to R-band o Aperture (cm): 45 o f-ratio: 1.9 o FOV: Sensitivity (magnitude): Slew time: < 10 s ROTSE-IIIb HET ROTSE-IIIb 1 December 2017 SMU PHYSICS McDonald Observatory Davis Mountains, West 34 Texas
35 Dwarf Novae 1 December 2017 SMU PHYSICS An artist's concept of the accretion disk around the binary star WZ Sge. Using data from Kitt Peak National Observatory and N Spitzer Space Telescope, a new picture of this system 35 has emerg which includes an asymmetric outer disk of dark matter.
36 ROTSE3 J Damien 1 st detection (110706): o ROTSE-IIIb & ROTSE-IIId o ATel #2126 Outburst ( ): o ROTSE-IIIb o ATel #5449 Magnitude (max): 16.6 (RA, Dec) = (20:32:25.01, +60:28:36.59) UG Dwarf Nova o o o Close binary system consisting of a red dwarf, a white dwarf, & an accretion disk surrounding the white dwarf Brightening by 2-6 magnitudes caused by instability in the disk Disk material infalls onto white dwarf 1 December 2017 SMU PHYSICS 36
37 Novae (classical) Novae typically originate in binary systems containing sun-like stars, as shown in this artist's rendering. 1 December 2017 SMU PHYSICS 37
38 M33N a 1 st detection: (ROTSE-IIIb) (RA, Dec) = (01:32:57.3, +30:24:27) Constellation: Triangulum Host galaxy: M33 Magnitude (max): 16.6 z = (~0.85 Mpc, ~2.7 Mly) Classical nova o Explosive nuclear burning of white dwarf surface from accumulated material from the secondary o Causes binary system to brighten 7-16 magnitudes in a matter of 1 to 100s days o After outburst, star fades slowly to initial brightness over years or decades CBET December 2017 M33 Triangulum Galaxy 38
39 1 December 2017 SMU PHYSICS 39
40 Supernovae Supernovae Search SN 2012ha SN 2013X M a (nova) ROTSE3 J (dwarf nova) SN 2013ej (M74) SN 1994D (NGC 4526) 1 December 2017 SN 2013ej (M74) 40
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43 SN 2012cg (NGC 4424) 1 December 2017 SMU PHYSICS 43
44 SN 2012ha ( Sherpa ) 1 st detection: (ROTSE-IIIb) Type: Ia-normal o Electron degeneracy prevents collapse to neutron star o Single degenerate progenitor: C-O white dwarf in binary system accretes mass from companion (main sequence star) o Mass Chandrasekhar limit (1.44 M ) o Thermonuclear runaway o Deflagration or detonation? o Standardizable candles acceleration of expansion dark energy Magnitude (max): 15.0 Observed 1 month past peak brightness (RA, Dec) = (13:00:36.10, +27:34:24.64) Constellation: Coma Berenices Host galaxy: PGC z = (~75 Mpc; ~240 Mly) CBET 3319 SN 2012ha: HET finder scope SMU PHYSICS 44
45 SN 2013X ( Everest ) Discovered (ROTSE-IIIb) Type Ia 91T-like o Overluminous o White dwarf merger? o Double degenerate progenitor? Magnitude (max): 17.7 Observed 10 days past maximum brightness (RA, Dec) = (12:17:15.19, +46:43:35.94) Constellation: Ursa Major Host galaxy: PGC z = (~140 Mpc; ~450 Mly) CBET 3413 SMU PHYSICS 45
46 What happens to a stellar core more massive than 1.44 solar masses? 1. There aren t any 2. They shrink to zero size 3. They explode 4. They become something else 1 December 2017 SMU PHYSICS 46
47 Neutron Stars Extremely compact: ~ 10 km radius Extreme density: 1 teaspoon would weigh ~ 10 9 tons (~ as much as all the buildings in Manhattan) Spin rapidly: up to 600 rev/s Pulsars High magnetic fields (~ T): Compressed from magnetic field of progenitor star An artist s rendering of a neutron star compared with the skyline of Chicago. Neutron stars are about 12 miles in diameter and are extremely dense. CreditDaniel Schwen/Northwestern, via LIGO-Virgo 1 December 2017 SMU PHYSICS 47
48 Neutron Stars Degenerate stellar cores heavier than 1.44 solar masses collapse to become neutron stars Formed in supernovae explosions Electrons are not separate Combine with nuclei to form neutrons Neutron stars are degenerate Fermi gas of neutrons Near the center of the Crab Nebula is a neutron star that rotates 30 times per second. Photo Courtesy of NASA. 1 December 2017 SMU PHYSICS 48
49 Neutron Energy Levels Only two neutrons (one up, one down) can go into each energy level In a degenerate gas, all low energy levels are filled Neutrons have kinetic energy, and therefore are in motion & exert pressure even if temperature is zero Neutron stars are supported by neutron degeneracy 1 December 2017 SMU PHYSICS 49
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52 Magnetars 1 December 2017 SMU PHYSICS 52
53 GW This illustration depicts the first moments after a neutron-star merger. A jet of gamma rays erupts perpendicular to the orbital plane, while radioactively heated ejecta glow in multiple wavelengths. Credit: NSF/LIGO/Sonoma State University/A. Simonnet The Swope and Magellan Telescopes in Chile captured the first optical and near-ir images of the aftermath of the 17 August neutron-star collision. Over four days the source became dimmer and redder. Credit: 1M2H/UC Santa Cruz and Carnegie Observatories/Ryan Foley The two LIGO detectors measured a clear signal from the merging neutron stars. Virgo data helped localize the source. Credit: B. P. Abbott et al., Phys. Rev. Lett., December 2017 SMU PHYSICS National Optical Astronomy Observatory Detection by LIGO Hanford, LIGO Livingston, & Virgo (Italy) 3 LIGO detectors enabled triangulation of event to be within 60 square degrees Much improved over previous binary black hole mergers (600 square degrees) Chirps lasted 1.5 min, 3300 oscillations GRB : Detection of short-duration GRB (kilonova) by Fermi & INTEGRAL satellites 1.7 s after GW detection Followed by ground-based observations by 70+ telescopes in Southern Hemisphere Both GW & EM (γ-ray, X-ray, UV, optical, IR, radio) event NGC 4993, 40 Mpc Binary neutron star merger 1.6 M S neutron star merged with 1.1 M S neutron star = 2.7 M S neutron star (or black hole) End product: Black hole or fat neutron star? Origin of heavy elements Ag, Pt, Au, & U by nuclear r-process Produced ~10 4 Earth masses of elements heavier than Fe; Earth masses of Au Crucible of cosmic alchemy Era of multi-messenger astronomy begins! 53
This class: Life cycle of high mass stars Supernovae Neutron stars, pulsars, pulsar wind nebulae, magnetars Quark-nova stars Gamma-ray bursts (GRBs)
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