1 Astronomy 102, Fall 2001 16 October 2001 The remnant of supernova 1987A in the Large Magellanic Cloud, seen by the Hubble Space Telescope in 1995 (NASA/STScI). Today in Astronomy 102: neutron degeneracy pressure and neutron stars The relativity of mass Neutron stars and the Oppenheimer maximum mass. Collapse of burned- out stars, the formation of neutron stars, and supernovae. Pulsars are neutron stars. When is black-hole formation inevitable?
Today in Astronomy 102: neutron degeneracy pressure and neutron stars
Dec 30, 2015
Today in Astronomy 102: neutron degeneracy pressure and neutron stars. The relativity of mass Neutron stars and the Oppenheimer maximum mass. Collapse of burned-out stars, the formation of neutron stars, and supernovae. Pulsars are neutron stars. When is black-hole formation inevitable?. - PowerPoint PPT Presentation
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1Astronomy 102, Fall 200116 October 2001
The remnant of supernova 1987A in the Large Magellanic Cloud, seen by the Hubble Space Telescope in 1995 (NASA/STScI).
Today in Astronomy 102: neutron degeneracy pressure and neutron stars The relativity of mass Neutron stars and the
Oppenheimer maximum mass.
Collapse of burned-out stars, the formation of neutron stars, and supernovae.
Pulsars are neutron stars.
When is black-hole formation inevitable?
16 October 2001 Astronomy 102, Fall 2001 2
The maximum mass and the speed-of-light limit
Why is the speed of light the maximum speed that can be reached by any moving body? (Remember, this was not part of the two original axioms from which Einstein started…) Because of the relativity of mass: if a body with
rest mass m0 moves at speed V with respect to an observer, the observer will measure a mass
for the body. (Another result of the Special Theory.) Note similarity to the formula for time dilation: in
particular, that the denominator approaches 0, and thus m approaches infinity, if V approaches c.
02
2
.
1
mm
V
c
16 October 2001 Astronomy 102, Fall 2001 3
The maximum mass and the speed-of-light limit (continued)
So, suppose you have a body moving at very nearly the speed of light, and you want it to exceed the speed of light. What can you do? It needs to accelerate for its speed to increase. You need to exert a force on it in order to make it
accelerate. The force required is, essentially, proportional to
the product of mass and acceleration in your reference frame. (Nonrelativistic version of this statement is Newton’s second law: force = mass times acceleration.)
But the mass approaches infinity as V approaches c, and thus an infinite force is required to accelerate it further. There’s no such thing as an infinite force, so c is the ultimate speed limit.
16 October 2001 Astronomy 102, Fall 2001 4
Final collapse of burned-out stars
Electron degeneracy pressure can hold up a star of mass 1.4M or less against its weight, and do so indefinitely. Stellar cores in this mass range at death become white dwarfs.For heavier stars: gravity overwhelms electron degeneracy pressure, and the collapse doesn’t stop with the star at planet size. As the star is crushed past a circumference of 104
cm or so, all the electrons and protons in the star are squeezed together so closely that they rapidly combine to form neutrons:
Eventually, then, the collapse might be stopped by the onset of neutron degeneracy pressure.
A star whose weight is held up by neutron degeneracy pressure is called a neutron star.
.ep e E n
16 October 2001 Astronomy 102, Fall 2001 5
Oppenheimer’s theory of neutron stars
Neutron stars were first proposed to exist, and to cause supernovae by their formation, by Zwicky and Baade (1934).First calculations of their sizes: Landau (1938). Neutron stars are analogous to white dwarfs, but the
calculations are much more difficult, since the strong nuclear force and general relativity must be taken into account. (For white dwarfs, special relativity suffices because the gravity of these stars is not strong enough to make general relativistic effects substantial.)
As such, they may also be expected to have a maximum mass, as white dwarfs do. For stars more massive than this maximum, neutron degeneracy pressure will not prevent the formation of black holes.
16 October 2001 Astronomy 102, Fall 2001 6
Albert Einstein and J. Robert Oppenheimer at Caltech in 1939. They probably were, at that moment, discussing the prevention of black holes by neutron-star formation.
Oppenheimer’s theory of neutron stars (cont’d)
First calculation of maximum mass: Oppenheimer and Volkoff (1939). They got 0.7M; more recent calculations, with improvements in the expression of the nuclear forces, give 1.5-3 M. (We will use 2M in this course.)
16 October 2001 Astronomy 102, Fall 2001 7
0.01 0.1 1 100
200
400
600
Model neutron star40 Eri B and Sirius BRochester's circumference
Mass (solar masses)
Cir
cum
fere
nce
(km
)
Circumference ofRochester (outerloop)
Maximum mass 2M
Oppenheimer’s theory of neutron stars (cont’d)
Updated calculation using 1990s-vintage inputs for the strong nuclear force; otherwise the same as Oppenheimer and Volkoff.
Cir
cum
fere
nce
(km
)
Mass M
16 October 2001 Astronomy 102, Fall 2001 8
0.01 0.1 1 10110
5
1106
1107
1108
1109
11010
11011
Z/A = 0.5 white dwarfNeutron starRochester's circumferenceEarth's circumferenceBlack hole horizon
Mass (solar masses)
Cir
cum
fere
nce
(cm
)
White dwarfs, neutron stars and black hole horizons
Rochester
Earth
WD
NSBH
Cir
cum
fere
nce
(cm
)
Mass M
16 October 2001 Astronomy 102, Fall 2001 9
Implications of neutron stars: (Type II) supernovae
After the electron degeneracy pressure is overpowered, and the electrons and protons combine to form neutrons, the star is free to collapse under its weight. Nothing can slow down this collapse until the neutrons are close enough together for degeneracy to set in. • Requires confinement to space a factor of order
1000 smaller than for electron degeneracy pressure. This collapse takes very little time, and the collapsing
material is moving very fast when neutron degeneracy pressure takes over.
A neutron-degeneracy-pressure supported core can form from the inner part of the collapsing material.
The outer, collapsing material that didn’t make it into the neutron core proceeds to bounce off this core, rebounding into the rest of the star and exploding with great violence.
16 October 2001 Astronomy 102, Fall 2001 10
A supernova forms from a dead, massive star
(not drawn to scale)
Star: 6 M, 107 km circumferenceCore: 1.4 M, 105 km circumference
Core: 104 km circum-ference. Electrons and protons begin combining to form neutrons.
2 years
16 October 2001 Astronomy 102, Fall 2001 11
A supernova forms from a dead, massive star (continued)
Core: 70 km circumference,neutron degeneracy pressuresets in.
Core: 104 km circumference. Electrons and protons begin combining to form neutrons.
1.2 seconds
16 October 2001 Astronomy 102, Fall 2001 12
A supernova forms from a dead, massive star (continued)
Core: 70 km circumference,neutron degeneracy pressure sets in. This makes the core very stiff.Outside of core: still collapsing, moving inwards at about 1010 cm/s. (Near light speed!) Bounces off stiff core.
16 October 2001 Astronomy 102, Fall 2001 13
A supernova forms from a dead, massive star (continued)
Core: Still 70 km circumference, it is now stable.
Outside of core: the rebounding outer-star material explodes the rest of the star. Energy comes from bounce, and from gravitational energy of core.
A few seconds
16 October 2001 Astronomy 102, Fall 2001 14
A supernova forms from
a dead, massive star (continued)
Neutron star
About a day
Expanding supernovashell. Very, very bright for about a month after explosion (can outshine rest of galaxy!).
15Astronomy 102, Fall 200116 October 2001
Mid-lecture break
Be on the lookout, on your email, for a notice of the availability of Homework Set #4 on WeBWorK.
Image of Supernova 1994D in the galaxy NGC 4526, taken a few weeks after it was first discovered in March 1994, by the High-z Supernova Search Team, with the NASA Hubble Space Telescope.Supernova
16Astronomy 102, Fall 200116 October 2001
Supernova 1987A
Before: the Tarantula Nebula in the Large Magellanic Cloud, in 1984. The star that exploded is indicated by the white arrow.After: the same field, two weeks after the supernova went off. It was still easily visible to the naked eye.Images by David Malin, Anglo-Australian Observatory.
17Astronomy 102, Fall 200116 October 2001
The appearance of a supernova as time passes
Here is an animated view of the first month after the explosion of a supernova, courtesy of UC Berkeley’s Supernova Cosmology Project (Perlmutter, Nugent, Conley, Nugent).
Click on image to see movie.
16 October 2001 Astronomy 102, Fall 2001 18
Neutron stars, supernovae and pulsars
Many hundreds of neutron stars are known today; they appear mostly as pulsars: pulsating, starlike sources of radio and visible light, discovered in 1967 by Jocelyn Bell. The Oppenheimer-Volkoff theory of neutron stars, and
their maximum mass, has been confirmed in all essentials.
Theory and experiment on nuclear matter at high density done largely through the US and USSR nuclear weapons development programs.
Astronomers have only been able to measure the masses of a handful of neutron stars; they all turn out to be around 1.4-1.5M, comfortably less than 2M.
16 October 2001 Astronomy 102, Fall 2001 19
Neutron stars, supernovae and pulsars (continued)
The Zwicky theory of supernova explosion by neutron-star formation has basically been confirmed.
Many pulsars are seen to be associated with supernova remnants.• Notably the Crab pulsar and nebula, in Taurus,
remnants of Supernova 1054. Not all live stars in the neutron-star mass range
will become neutron stars; many eject a large fraction of their mass in their final stages of life and make the white dwarf cutoff.• In their final “mass loss” stage, light from the
stellar core lights up the ejected material, producing a planetary nebula.
20Astronomy 102, Fall 200116 October 2001
Pulsar
16 October 2001 Astronomy 102, Fall 2001 21
A neutron star observed directly
The neutron star at the center of the Crab Nebula, the remnant of the supernova visible in the year 1054. It is seen as a pulsar in these images taken 0.03 second apart. (This image’s orientation is rotated counterclockwise about 100o from the previous one.)
On
Off
16 October 2001 Astronomy 102, Fall 2001 22
0.01 0.1 1 10110
5
1106
1107
1108
1109
11010
11011
Z = 0.5 white dwarfNeutron starBlack hole
Mass (solar masses)
Cir
cum
fere
nce
(cm
)
Final collapse of burned-out stars: white dwarf, neutron star, or black hole?
If these stars do not eject mass while in their death throes, their fates are as follows: the Sun will become a white dwarf, Procyon will become a neutron star, and Sirius A will become a black hole.
Su
nP
rocyon
Sir
ius A
Cir
cum
fere
nce
(cm
)
Mass M
WD
NS
BH
16 October 2001 Astronomy 102, Fall 2001 23
Summary: status of the Schwarzschild singularity and black holes
Electron and neutron degeneracy pressure can prevent the formation of black holes from dead stars, but only for masses below about 2M.
Stars with masses in excess of this must eject material during their final stages of life if they are to become white dwarfs or neutron stars. (Most do.)
For masses larger than this, no force known to science exists that would prevent the collapse from proceeding to the formation of a black hole. For very heavy stars, black hole formation is probably compulsory. (Einstein’s objections are overruled.)
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