Is the moon's orbit circularizing? Why does tidal heating circularize orbits?
The moon has an elliptical orbit (of course), but as it inches away from the Earth each year, does its orbit become more circular and how come? Io's orbit is becoming more circular due to tidal heating effects, but why?
the-moon
add a comment |
The moon has an elliptical orbit (of course), but as it inches away from the Earth each year, does its orbit become more circular and how come? Io's orbit is becoming more circular due to tidal heating effects, but why?
the-moon
Suggestion: go to HORIZONS, compute the Moon's osculating elements wrt Earth for the largest possible time range and see if the eccentricity changes a lot.
– barrycarter
2 hours ago
add a comment |
The moon has an elliptical orbit (of course), but as it inches away from the Earth each year, does its orbit become more circular and how come? Io's orbit is becoming more circular due to tidal heating effects, but why?
the-moon
The moon has an elliptical orbit (of course), but as it inches away from the Earth each year, does its orbit become more circular and how come? Io's orbit is becoming more circular due to tidal heating effects, but why?
the-moon
the-moon
edited 3 hours ago
asked 3 hours ago
ElectricSupernova
40619
40619
Suggestion: go to HORIZONS, compute the Moon's osculating elements wrt Earth for the largest possible time range and see if the eccentricity changes a lot.
– barrycarter
2 hours ago
add a comment |
Suggestion: go to HORIZONS, compute the Moon's osculating elements wrt Earth for the largest possible time range and see if the eccentricity changes a lot.
– barrycarter
2 hours ago
Suggestion: go to HORIZONS, compute the Moon's osculating elements wrt Earth for the largest possible time range and see if the eccentricity changes a lot.
– barrycarter
2 hours ago
Suggestion: go to HORIZONS, compute the Moon's osculating elements wrt Earth for the largest possible time range and see if the eccentricity changes a lot.
– barrycarter
2 hours ago
add a comment |
1 Answer
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Short answer: YES.
In general, tidal forces in binary systems (like the Earth-Moon system, or a binary star, etc...) effect the binary in three main ways: in order of longest timescale to shortest timescale
1) circularization of the orbit (eccentricity goes to zero, binary separation goes to minimum).
2) alignment of the binary components' spin angular momenta with the orbital angular momentum (the directions of $S$ and $L$ are the same).
3) synchronization of the binary components' spin angular momenta with the orbital angular momentum (the magnitudes of $S$ and $L$ are the same).
but why?
There's different ways of answering "why," and here is a great conceptual answer given by the God Father of astrophysical tides himself, Z. P. Zahn:
A fundamental property of closed mechanical systems is that they conserve their
total momentum. This is true in particular for binary stars, star-planet(s) systems,
whether they possess or not a circumstellar disc, if one can ignore the angular
momentum that is carried away by winds and by gravitational waves. Through
tidal interaction, kinetic energy and angular momentum are exchanged between
the rotation of the components their orbital motion and the disc. In the absence
of such a disc, which is the case that we shall consider here, they evolve due
to viscous and radiative dissipation to the state of minimum kinetic energy, in
which the orbit is circular, the rotation of both stars is synchronized with the
orbital motion, and their spin axis are perpendicular to the orbital plane. How
rapidly the system tends to that state is determined by the strength of the tidal
interaction, and thus by the separation of the two components...
So, basically, the tidal torque drives dissipation, and this dissipation brings the binary to a minimum kinetic energy state, i.e. circular orbit, synchronized spins with the orbit, aligned spins with the orbit.
Here's a contour plot of the timescales provided by equations #$9 - 13$ from Hut's 1981 seminal paper, assuming the separation does not change much relative to the angular momenta, for a binary composed of a black hole and a Wolf-Rayet star, which is a similar system to a planet-satellite system, where the timescales are parameterized in terms of the mass of the WR star and the separation of the binary:
The dotted black line is the merger timescale for the binary due to gravitational waves, meaning below that line you are binary that mergers within the lifetime of the universe. The synchronization timescale is independent of the initial spin of the WR star, which is why there is only one synchronization line in the plot, but the alignemnt timescale does depend on the initial spin of the component feeling the tides. Points below the contours achieve that process (below the red dashed line are synchronized). The quantity $f_{B}$ is the break-up fraction parameter, is between $0$ and $1$, and the choice of which determines the initial WR star spin as a fraction of its break-up spin. (the tidal timescale contours were made by equating the WR lifetime with the tidal timescale).
Lastly, it must be said that a WR star is quite different from a moon/satellite, however the effects of tides on each is similar enough to make a conceptual comparison (since a WR star is much less massive than the BH, as is the moon than the Earth, the hierarchy of tidal timescales is the same, but you must keep in mind that the WR's apsidal response to the tidal gradient is very different than a rocky moon's). Also, as you pointed out the Moon does have an eccentric orbit, but the moon is also tidally synchronized with the Earth's rotation (which are both sync'ed to the orbital rotation). This should make sense since it takes longer for tides to circularize than to synchronize.
I'm sure somebody can post an example of using tides in an actual planet-moon system, rather than my black hole-star system. :)
Sorry, I had the incorrect graph attached at first.
– N. Steinle
1 hour ago
add a comment |
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Short answer: YES.
In general, tidal forces in binary systems (like the Earth-Moon system, or a binary star, etc...) effect the binary in three main ways: in order of longest timescale to shortest timescale
1) circularization of the orbit (eccentricity goes to zero, binary separation goes to minimum).
2) alignment of the binary components' spin angular momenta with the orbital angular momentum (the directions of $S$ and $L$ are the same).
3) synchronization of the binary components' spin angular momenta with the orbital angular momentum (the magnitudes of $S$ and $L$ are the same).
but why?
There's different ways of answering "why," and here is a great conceptual answer given by the God Father of astrophysical tides himself, Z. P. Zahn:
A fundamental property of closed mechanical systems is that they conserve their
total momentum. This is true in particular for binary stars, star-planet(s) systems,
whether they possess or not a circumstellar disc, if one can ignore the angular
momentum that is carried away by winds and by gravitational waves. Through
tidal interaction, kinetic energy and angular momentum are exchanged between
the rotation of the components their orbital motion and the disc. In the absence
of such a disc, which is the case that we shall consider here, they evolve due
to viscous and radiative dissipation to the state of minimum kinetic energy, in
which the orbit is circular, the rotation of both stars is synchronized with the
orbital motion, and their spin axis are perpendicular to the orbital plane. How
rapidly the system tends to that state is determined by the strength of the tidal
interaction, and thus by the separation of the two components...
So, basically, the tidal torque drives dissipation, and this dissipation brings the binary to a minimum kinetic energy state, i.e. circular orbit, synchronized spins with the orbit, aligned spins with the orbit.
Here's a contour plot of the timescales provided by equations #$9 - 13$ from Hut's 1981 seminal paper, assuming the separation does not change much relative to the angular momenta, for a binary composed of a black hole and a Wolf-Rayet star, which is a similar system to a planet-satellite system, where the timescales are parameterized in terms of the mass of the WR star and the separation of the binary:
The dotted black line is the merger timescale for the binary due to gravitational waves, meaning below that line you are binary that mergers within the lifetime of the universe. The synchronization timescale is independent of the initial spin of the WR star, which is why there is only one synchronization line in the plot, but the alignemnt timescale does depend on the initial spin of the component feeling the tides. Points below the contours achieve that process (below the red dashed line are synchronized). The quantity $f_{B}$ is the break-up fraction parameter, is between $0$ and $1$, and the choice of which determines the initial WR star spin as a fraction of its break-up spin. (the tidal timescale contours were made by equating the WR lifetime with the tidal timescale).
Lastly, it must be said that a WR star is quite different from a moon/satellite, however the effects of tides on each is similar enough to make a conceptual comparison (since a WR star is much less massive than the BH, as is the moon than the Earth, the hierarchy of tidal timescales is the same, but you must keep in mind that the WR's apsidal response to the tidal gradient is very different than a rocky moon's). Also, as you pointed out the Moon does have an eccentric orbit, but the moon is also tidally synchronized with the Earth's rotation (which are both sync'ed to the orbital rotation). This should make sense since it takes longer for tides to circularize than to synchronize.
I'm sure somebody can post an example of using tides in an actual planet-moon system, rather than my black hole-star system. :)
Sorry, I had the incorrect graph attached at first.
– N. Steinle
1 hour ago
add a comment |
Short answer: YES.
In general, tidal forces in binary systems (like the Earth-Moon system, or a binary star, etc...) effect the binary in three main ways: in order of longest timescale to shortest timescale
1) circularization of the orbit (eccentricity goes to zero, binary separation goes to minimum).
2) alignment of the binary components' spin angular momenta with the orbital angular momentum (the directions of $S$ and $L$ are the same).
3) synchronization of the binary components' spin angular momenta with the orbital angular momentum (the magnitudes of $S$ and $L$ are the same).
but why?
There's different ways of answering "why," and here is a great conceptual answer given by the God Father of astrophysical tides himself, Z. P. Zahn:
A fundamental property of closed mechanical systems is that they conserve their
total momentum. This is true in particular for binary stars, star-planet(s) systems,
whether they possess or not a circumstellar disc, if one can ignore the angular
momentum that is carried away by winds and by gravitational waves. Through
tidal interaction, kinetic energy and angular momentum are exchanged between
the rotation of the components their orbital motion and the disc. In the absence
of such a disc, which is the case that we shall consider here, they evolve due
to viscous and radiative dissipation to the state of minimum kinetic energy, in
which the orbit is circular, the rotation of both stars is synchronized with the
orbital motion, and their spin axis are perpendicular to the orbital plane. How
rapidly the system tends to that state is determined by the strength of the tidal
interaction, and thus by the separation of the two components...
So, basically, the tidal torque drives dissipation, and this dissipation brings the binary to a minimum kinetic energy state, i.e. circular orbit, synchronized spins with the orbit, aligned spins with the orbit.
Here's a contour plot of the timescales provided by equations #$9 - 13$ from Hut's 1981 seminal paper, assuming the separation does not change much relative to the angular momenta, for a binary composed of a black hole and a Wolf-Rayet star, which is a similar system to a planet-satellite system, where the timescales are parameterized in terms of the mass of the WR star and the separation of the binary:
The dotted black line is the merger timescale for the binary due to gravitational waves, meaning below that line you are binary that mergers within the lifetime of the universe. The synchronization timescale is independent of the initial spin of the WR star, which is why there is only one synchronization line in the plot, but the alignemnt timescale does depend on the initial spin of the component feeling the tides. Points below the contours achieve that process (below the red dashed line are synchronized). The quantity $f_{B}$ is the break-up fraction parameter, is between $0$ and $1$, and the choice of which determines the initial WR star spin as a fraction of its break-up spin. (the tidal timescale contours were made by equating the WR lifetime with the tidal timescale).
Lastly, it must be said that a WR star is quite different from a moon/satellite, however the effects of tides on each is similar enough to make a conceptual comparison (since a WR star is much less massive than the BH, as is the moon than the Earth, the hierarchy of tidal timescales is the same, but you must keep in mind that the WR's apsidal response to the tidal gradient is very different than a rocky moon's). Also, as you pointed out the Moon does have an eccentric orbit, but the moon is also tidally synchronized with the Earth's rotation (which are both sync'ed to the orbital rotation). This should make sense since it takes longer for tides to circularize than to synchronize.
I'm sure somebody can post an example of using tides in an actual planet-moon system, rather than my black hole-star system. :)
Sorry, I had the incorrect graph attached at first.
– N. Steinle
1 hour ago
add a comment |
Short answer: YES.
In general, tidal forces in binary systems (like the Earth-Moon system, or a binary star, etc...) effect the binary in three main ways: in order of longest timescale to shortest timescale
1) circularization of the orbit (eccentricity goes to zero, binary separation goes to minimum).
2) alignment of the binary components' spin angular momenta with the orbital angular momentum (the directions of $S$ and $L$ are the same).
3) synchronization of the binary components' spin angular momenta with the orbital angular momentum (the magnitudes of $S$ and $L$ are the same).
but why?
There's different ways of answering "why," and here is a great conceptual answer given by the God Father of astrophysical tides himself, Z. P. Zahn:
A fundamental property of closed mechanical systems is that they conserve their
total momentum. This is true in particular for binary stars, star-planet(s) systems,
whether they possess or not a circumstellar disc, if one can ignore the angular
momentum that is carried away by winds and by gravitational waves. Through
tidal interaction, kinetic energy and angular momentum are exchanged between
the rotation of the components their orbital motion and the disc. In the absence
of such a disc, which is the case that we shall consider here, they evolve due
to viscous and radiative dissipation to the state of minimum kinetic energy, in
which the orbit is circular, the rotation of both stars is synchronized with the
orbital motion, and their spin axis are perpendicular to the orbital plane. How
rapidly the system tends to that state is determined by the strength of the tidal
interaction, and thus by the separation of the two components...
So, basically, the tidal torque drives dissipation, and this dissipation brings the binary to a minimum kinetic energy state, i.e. circular orbit, synchronized spins with the orbit, aligned spins with the orbit.
Here's a contour plot of the timescales provided by equations #$9 - 13$ from Hut's 1981 seminal paper, assuming the separation does not change much relative to the angular momenta, for a binary composed of a black hole and a Wolf-Rayet star, which is a similar system to a planet-satellite system, where the timescales are parameterized in terms of the mass of the WR star and the separation of the binary:
The dotted black line is the merger timescale for the binary due to gravitational waves, meaning below that line you are binary that mergers within the lifetime of the universe. The synchronization timescale is independent of the initial spin of the WR star, which is why there is only one synchronization line in the plot, but the alignemnt timescale does depend on the initial spin of the component feeling the tides. Points below the contours achieve that process (below the red dashed line are synchronized). The quantity $f_{B}$ is the break-up fraction parameter, is between $0$ and $1$, and the choice of which determines the initial WR star spin as a fraction of its break-up spin. (the tidal timescale contours were made by equating the WR lifetime with the tidal timescale).
Lastly, it must be said that a WR star is quite different from a moon/satellite, however the effects of tides on each is similar enough to make a conceptual comparison (since a WR star is much less massive than the BH, as is the moon than the Earth, the hierarchy of tidal timescales is the same, but you must keep in mind that the WR's apsidal response to the tidal gradient is very different than a rocky moon's). Also, as you pointed out the Moon does have an eccentric orbit, but the moon is also tidally synchronized with the Earth's rotation (which are both sync'ed to the orbital rotation). This should make sense since it takes longer for tides to circularize than to synchronize.
I'm sure somebody can post an example of using tides in an actual planet-moon system, rather than my black hole-star system. :)
Short answer: YES.
In general, tidal forces in binary systems (like the Earth-Moon system, or a binary star, etc...) effect the binary in three main ways: in order of longest timescale to shortest timescale
1) circularization of the orbit (eccentricity goes to zero, binary separation goes to minimum).
2) alignment of the binary components' spin angular momenta with the orbital angular momentum (the directions of $S$ and $L$ are the same).
3) synchronization of the binary components' spin angular momenta with the orbital angular momentum (the magnitudes of $S$ and $L$ are the same).
but why?
There's different ways of answering "why," and here is a great conceptual answer given by the God Father of astrophysical tides himself, Z. P. Zahn:
A fundamental property of closed mechanical systems is that they conserve their
total momentum. This is true in particular for binary stars, star-planet(s) systems,
whether they possess or not a circumstellar disc, if one can ignore the angular
momentum that is carried away by winds and by gravitational waves. Through
tidal interaction, kinetic energy and angular momentum are exchanged between
the rotation of the components their orbital motion and the disc. In the absence
of such a disc, which is the case that we shall consider here, they evolve due
to viscous and radiative dissipation to the state of minimum kinetic energy, in
which the orbit is circular, the rotation of both stars is synchronized with the
orbital motion, and their spin axis are perpendicular to the orbital plane. How
rapidly the system tends to that state is determined by the strength of the tidal
interaction, and thus by the separation of the two components...
So, basically, the tidal torque drives dissipation, and this dissipation brings the binary to a minimum kinetic energy state, i.e. circular orbit, synchronized spins with the orbit, aligned spins with the orbit.
Here's a contour plot of the timescales provided by equations #$9 - 13$ from Hut's 1981 seminal paper, assuming the separation does not change much relative to the angular momenta, for a binary composed of a black hole and a Wolf-Rayet star, which is a similar system to a planet-satellite system, where the timescales are parameterized in terms of the mass of the WR star and the separation of the binary:
The dotted black line is the merger timescale for the binary due to gravitational waves, meaning below that line you are binary that mergers within the lifetime of the universe. The synchronization timescale is independent of the initial spin of the WR star, which is why there is only one synchronization line in the plot, but the alignemnt timescale does depend on the initial spin of the component feeling the tides. Points below the contours achieve that process (below the red dashed line are synchronized). The quantity $f_{B}$ is the break-up fraction parameter, is between $0$ and $1$, and the choice of which determines the initial WR star spin as a fraction of its break-up spin. (the tidal timescale contours were made by equating the WR lifetime with the tidal timescale).
Lastly, it must be said that a WR star is quite different from a moon/satellite, however the effects of tides on each is similar enough to make a conceptual comparison (since a WR star is much less massive than the BH, as is the moon than the Earth, the hierarchy of tidal timescales is the same, but you must keep in mind that the WR's apsidal response to the tidal gradient is very different than a rocky moon's). Also, as you pointed out the Moon does have an eccentric orbit, but the moon is also tidally synchronized with the Earth's rotation (which are both sync'ed to the orbital rotation). This should make sense since it takes longer for tides to circularize than to synchronize.
I'm sure somebody can post an example of using tides in an actual planet-moon system, rather than my black hole-star system. :)
edited 1 hour ago
answered 2 hours ago
N. Steinle
3219
3219
Sorry, I had the incorrect graph attached at first.
– N. Steinle
1 hour ago
add a comment |
Sorry, I had the incorrect graph attached at first.
– N. Steinle
1 hour ago
Sorry, I had the incorrect graph attached at first.
– N. Steinle
1 hour ago
Sorry, I had the incorrect graph attached at first.
– N. Steinle
1 hour ago
add a comment |
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Suggestion: go to HORIZONS, compute the Moon's osculating elements wrt Earth for the largest possible time range and see if the eccentricity changes a lot.
– barrycarter
2 hours ago