Alternate Planets, Suns, Stars, and Solar Systems Thread

This picture is taken from one of Sean Raymond's Planet Planet articles, Cohorts of co-orbital planets.

What the article doesn't explain, however, is the basis for the question. In a solar system in which six rocky planets, each one the size of Earth and each one orbited by a single moon 1/4 its mass from a distance of 238,900 miles, orbit their sun from one same distance, would a 60-degree difference allow each of the "Earths" to spin in day-night cycles?
The other Earths are completely irrelevant in terms of tidal forces in that situation, so they won't cause any issues in terms of tidal locking. The more massive moons would likely cause the Earths to be tidally locked to their own moons, though. (There still would be a day night cycle there, though, it would just be close to a month long)

The larger moons cause roughly 20.3 times as much tidal force as our moon does (Due to the larger mass and same distance)
The closest other Earths cause 0.0000017 times as much tidal forces as our moon does.
 
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This picture is taken from one of Sean Raymond's Planet Planet articles, Cohorts of co-orbital planets.

What the article doesn't explain, however, is the basis for the question. In a solar system in which six rocky planets, each one the size of Earth and each one orbited by a single moon 1/4 its mass from a distance of 238,900 miles, orbit their sun from one same distance, would a 60-degree difference allow each of the "Earths" to spin in day-night cycles?
Um, what? Do I understand your question to be "can these six rocky planets, each one 60 degrees from its leading and trailing neighbors, rotate at all" as opposed I suppose to being tidally locked to turn one face to the Sun, and thus each other (they would be rotating, but only once a year).

With a hexagon 60 degree separation from each other, the straight line distance to the nearest neighbor leading and trailing is exactly the same a as the orbital radius--you can see the hexagon is composed of 6 equilateral triangles after all. So if these are "Earths," each body pretty near the spitting image of our own planet in mass and composition and 1 AU from the Sun, they are also 1 AU from each other.

That's a lot of distance. There is no question of a planet as small as Earth exerting major tidal force on another such planet that far away. After all the Sun itself is much much larger (a third of a million times more massive IIRC) and its tidal force is not much of a brake on Earth's current 24 hour spin--a lot more of the reduction from the primordial faster spin (some 20 hours or so, or maybe 22?) has been due to interactions with Luna.

Now the picture doesn't show any moons at all whereas Luna is a lot smaller than 1/4 Earth mass. If you mean radius, yeah, Luna is about 1/4 Earth's radius and thus diameters are in the same ratio of course. Which means it has around 1/64 Earth's volume, and is less dense, hence its mass is around 1/80 Earth mass, not 1/4. Throwing in moons that big would be pretty dicey; if you moved them farther out they'd be approaching the radius of the Hill Sphere for each Earth-like world versus the Sun. And in diameter they would look almost as big as their primaries too.

Again, having an extra Earth an AU ahead and another behind is not going to mess with the orbit of a moon similar to Luna at a similar distance from its bigger rocky primary.

What bothers me is that while this arrangement is clearly metastable, it would take very little distortion to make it unstable. For some reason or other, people who talk about such rosettes of planets don't think six similar sized bodies is enough, they say the minimum is seven. Anyway I don't see how seven or any number of even absolutely identical bodies placed at exactly the same angle separation from each other manages to remain stable despite perturbations. Even slight perturbations would lead to a cascade of each objects drifting out of position and fairly soon after that we'd have six, or seven, or whatever number, of planets each in their own separate orbits, more or less waltzing around each other.

I can now see someone else answering your question on the presumption you meant what you said about the moons, each being 1/4 an Earth mass, thus 20 times Luna's mass. Again--such big moons are problematic. But again, the leading and trailing Earths are not relevant to the problems you ask about, just as @Lyhoko Leaci says.
 
So? Why do you need a wide habitable zone in the first place? As far as I can tell, you're just imagining how a small number of species might radiate given a planet of their own, what does it matter if they're in the same star system or hundreds of different ones?

Because I'm imagining each of Earth's ecoregions, extant and prehistoric, on each habitable world.
 
Is it possible to have two moons in stable orbit of an Earth-sized terrestrial planet without apocalyptic tides, assuming the two moons together are equivalent in mass to one Luna?
 
Because I'm imagining each of Earth's ecoregions, extant and prehistoric, on each habitable world.
That still doesn't explain why each world needs to be in the same habitable zone. What does it matter if they're instead all orbiting stars bound loosely in some kind of globular cluster-like organization or, heck, just scattered over half the galaxy?
 
Because I'm imagining each of Earth's ecoregions, extant and prehistoric, on each habitable world.
If you want that and a single habitable zone, it's very easy for someone with full-scale orbital engineering abilities to construct rings and rings and rings of Earth-mass planets around even very low-mass stars. And it's not like a narrow habitable zone impedes the habitability of M-dwarf systems as much as you think- TRAPPIST-1 has at least 3 habzone planets, though if you hate resonances that obviously won't suffice. If you're willing to use lower-mass planets, then you can cram more in too.

Is it possible to have two moons in stable orbit of an Earth-sized terrestrial planet without apocalyptic tides, assuming the two moons together are equivalent in mass to one Luna?

Absolutely, even if they're closer in than Luna. Tides would be more complex, but likely not much higher. There's a calculator for tidal strength somewhere....
 
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Because I'm imagining each of Earth's ecoregions, extant and prehistoric, on each habitable world.
Six Earths as satellites of big big warm Jupiter is simple and possible solution. Different day cycles would be problem if you introduce life from Earth but no problems for life on those planets
 
Is it possible to have two moons in stable orbit of an Earth-sized terrestrial planet without apocalyptic tides, assuming the two moons together are equivalent in mass to one Luna?
@Rosella pretty well covered most of it. I'd stress two opposite constraints--to keep one moon's tide below Lunar levels, it can be bigger than Luna but then needs to orbit farther out, whereas the "Hill Sphere" is a limit on how far out it can be and still be in stable orbit around Earth. This is the radius where the gravitational force exerted by Earth's mass equals the tidal force of the Sun at that radius from Earth--tidal force rises linearly with radius, Earth's gravity falls at the inverse square, so it scales as the cube root of the ratio of mass of Earth to the Sun, and also linearly (for other planets, or imagining Earth moved to another orbital radius) with the distance of the planet from the Sun--that is the Hill sphere is actually a ratio applied to the orbital radius. At 10 AU it is ten times as great as at 1 AU. So we can't have any moon of any size at all without upper limit.

On the other hand, if you want to keep the magnitude of the tidal effect within a certain modest multiplier of the effect Luna has, it is well to remember the effect goes as the inverse cube of distance. So it is very important to consider the distance you propose each moon to orbit at. A moon of given mass has eight times the effect if it orbits at half the radius. Several moons much smaller than Luna put together can exert more severe tides on Earth than Luna, if they are a lot closer in. Meanwhile of course Earth is exerting a tide on them too, and that also rises steeply as each one orbits closer and drops if it recedes farther, again sharply. The actual acceleration as noted is a factor of the radius from the moon's center of mass, it is the rate at which that acceleration rises with that distance that varies with orbital distance measured to the center of mass.

Finally, the form of the tidal field resembles a dipole. Along the axis between the body exerting the tide's center of mass and that of the body affected, it tends to pull things away from the affected object's center of mass, but in the plane that this axis is normal to, running through the center of mass at right angles to that ray, the field actually compresses masses toward the center--at 1/2 the magnitude at a given distance. Between the ray between the centers of masses and this plane, the net field has both radial and angular components.

The upshot of this is that if we had two moons, one eight times the mass of the other but orbiting at twice the distance so its effect is identical in magnitude to the closer smaller moon, when they happen to line up (they probably do orbit in the same plane but they might not; if they do of course they line up periodically, once with both on the same side and then again with them , and even if they don't they might line up by coincidence) then their effects add, but if they are at 90 degrees to each other each one cancels out a portion (in this case identical) of the stretching effect on the main ray axis; the effect in the two perpendicular planes is more complicated, cancelling on one axis (in the plane both main rays lie in) and adding on the third axis. Thus, with these two moons, the net tidal effect is complicated. And of course both these moons' combined field is interacting with the Sun's tidal field too.

So if we have a set of moons designed to have their maximum tidal effects add up to the same magnitude as the Lunar field of OTL on Earth, in general tides will be weaker, if grouping all the moons on the same line happens rarely. Vice versa, you might get away with occasionally having tides much stronger than Luna exerts at maximum (which is roughly about twice the maximum effect the Sun ever exerts) but having them usually similar or less due to this mutual interference interaction.

And of course a habitable planet can probably handle tides considerably strong than a "spring tide" where Luna and Sol line up (happens twice a month). It means the water surges around more, and this is an influence that can contribute to overall geological heat, and can trigger earthquakes, volcanic eruptions, etc. And this represents power being dissipated and angular momentum being transferred between bodies; currently Earth's rotation is being slowed and the Moon is receding to ever higher orbit--Earth's spin angular momentum is transferred to Luna's orbital angular momentum, and some energy is transferred with it while other energy taken from Earth slowing down turns into heat. So I would guess magnitudes similar to what Earth endures currently are clearly fine but if we kick it up a factor of ten or more, that might have drastic effect on planet geology or time scales of changing spin rate, axis precession, orbital changes, etc. (This is one reason I always try to keep the magnitude similar, to avoid going into this unknown territory, also of course one wants to limit how drastic tidal effects are on the shores, how frequent and powerful earthquakes and volcanic eruptions are, etc.

Another thing about tides is that if a body is tidally locked, what matters is the rate at which material moves through changing tidal accelerations, not so much the actual magnitude of those fields. A body that is turning in phase with the field will change shape, becoming elongated on the main line of stretching force into a prolate spheroid (if it is fluid at all, but a habitable planet is probably mostly liquid outer core and plastic mantle-if we could magically turn on a powerful tide the surface would suffer badly as the planet shifts into its new equilibrium shape, but for ISOTs and so on one imagines the ASBs magically map the old planet onto the new spheroid and the crust is adjusted to the equilibrium of the fluid planet material below. Assuming this happens, liquids assume equipotential shapes so the egg shape is all one level gravitationally speaking. Of course we can imagine a formerly warm planet cooling off and freezing in a certain shape, and then the tidal effect weakening somehow, so we now have something like Larry Niven's imagined planet Jinx, with the ocean pooling around the short circumference and the Ends poking up out of the atmosphere--but if the tides that formed Jinx into that shape persisted, then the sea and air would coat the surface as though it were a sphere. (Sort of--the potential of the surface is the same, but the rate at which the potential changes as one goes upward varies depending on where one is on the egg shape, and that affects where the mass of air concentrates as lower rates of potential dropping provide more volume within a given potential range).

But the devil is in the details--I suspect it is impossible to ever have absolutely perfect tidal locking. There are perturbations acting on the system and these will tend to knock the spinning planet a bit out of whack with its orbit--in fact it is reactions from these mismatches that act to keep them largely in synch. And that means the tidal fields will not remain constant or stationary perfectly, and their fluctuations will act to move water around and so forth. So when I say for instance that you can have two Earthlike planets mutually orbiting each other with a 24 hour period, and that the massively stronger tide versus Luna's on Earth currently (they are closer to each other than Luna is to Earth, by a factor of 8 or so and thus if either were the size of Luna their tide would be 500 times stronger, but also each being Earthlike they mass 80 times more so it is 80 times 500, or 40,000 times stronger) these worlds having bearable tides depends on their staying very very closely in synch indeed; a half percent relative motion would result in tides 200 times stronger than Earth endures! Are such small relative motions, 1/200 of 1/200, adequate to keep their two spin axes lined up close enough to their shared orbital axis? I am not sure! The fact the forces get strong fast probably means they can stay in synch but perhaps it is a fact of life on any such worlds that the tidal phenomena are gigantic in magnitude, not 40,000 times what Earth experiences but maybe say 1000 times worse, or 100, or anyway 10. I don't honestly know for sure how it all works out, bearing in mind there will be strong interactions with third objects like the Sun.
 
And of course a habitable planet can probably handle tides considerably strong than a "spring tide" where Luna and Sol line up (happens twice a month). It means the water surges around more, and this is an influence that can contribute to overall geological heat, and can trigger earthquakes, volcanic eruptions, etc. And this represents power being dissipated and angular momentum being transferred between bodies; currently Earth's rotation is being slowed and the Moon is receding to ever higher orbit--Earth's spin angular momentum is transferred to Luna's orbital angular momentum, and some energy is transferred with it while other energy taken from Earth slowing down turns into heat. So I would guess magnitudes similar to what Earth endures currently are clearly fine but if we kick it up a factor of ten or more, that might have drastic effect on planet geology or time scales of changing spin rate, axis precession, orbital changes, etc. (This is one reason I always try to keep the magnitude similar, to avoid going into this unknown territory, also of course one wants to limit how drastic tidal effects are on the shores, how frequent and powerful earthquakes and volcanic eruptions are, etc.
It's not that unknown. Remember that the Moon formed much, much closer to Earth, possibly just beyond the Roche limit. At that distance (about four times the radius of Earth), the Moon would have exerted a tidal acceleration of approximately 4* 10^-3 m/s^2, which is pretty close to 4 000 times bigger than the current value. It wouldn't have dropped as low as merely ten times the current value until the Moon moved at least 25 or so Earth radii away from Earth, which would have taken somewhere between 500 million and a billion years to reach. Didn't seem to hurt the Earth that much...
 
Any habitable zone smaller than a yellow dwarf's is not "large".
A middling-luminosity G dwarf like Sol has a mildly optimistic habitable zone wide enough for three fairly widely spaced planets- 0.7 au. And I'm unsure what you want by "long-term"- a project like Serina only needs about two billion years to work within, which is short enough that even an F dwarf could be relatively stable luminosity-wise throughout that time.
 
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Because in looking for suitable, long-term habitable zones to seed Earth ecosystems in Serina-style, giant stars and dwarf binaries keep ending up short.
You don't need a quasar for that. If you want a good habitable zone, you'd want an F5V-F9V main sequence star which has one over 1 AU wide. They'll still live for 2-3 billion years on the main sequence (Procyon, an F5V star, for instance is about 2 billion years old and will evolve into a red giant in about 10 million years). Larger stars are more likely to form gas giants, which may be in the habitable zone. For instance, Iota Horologii (a G0V star slightly larger than the Sun) has a planet twice the size of Jupiter at around Earth's orbit. These gas giants are also more likely to be super-Jupiters or even brown dwarf companions which means Earth-size exomoons are more likely. This means you could easily pack in 2 or 3 planets in the habitable zone and maybe a few sizable worlds at the trojan points of those gas giants. Depending on the system, it's possible to have trojan planets in the size range between Mars and Earth but I don't think you'd be able to have, say, three gas giants each with a trojan planet at their L4-L5 point (for 6 trojan planets).

As for life around an F-type main sequence star, they'd be subject to higher levels of radiation from the star than Earth was which means that as long as an ozone layer developed early, there would be more incentive for life to both emerge and develop, since stellar radiation is one driver of evolution. And if you have several exomoons and trojan planets, it's very possible that abiogenesis on one world could seed much of that system with life. The 2-3 billion year "time limit" sucks, but we don't know if 4 billion years to have a "Cambrian explosion" type radiation of life is common or not. I think 1.5-2 billion years is possible for a Cambrian explosion type event. And if you want/have sentient life, evolving in a moon around a gas giant with an F-type main sequence star putting out far more energy than the Sun if you get up close is pretty much the single most optimal set-up possible.

Early F-type (F0V-F4V) or especially later A-type (A5V-A9V, like Altair) would be better in terms of every factor I mentioned above, but you're really pushing plausibility to have complex life evolve before the red giant phase (which is 1.3-2 billion years here). Although these star systems might work very well if you have life evolve in the ocean on a "snowball Earth" type moon outside the habitable zone. This would give several hundred million additional years for life to develop although there's going to be an issue with the atmosphere (not enough time for an oxygen atmosphere to develop). Early A-type stars wouldn't work without inserting already complex life onto planets and moons there, and B-type stars wouldn't work at all because the star is already a red giant by the time the planet cools from formation and anything above 8 solar masses (early B-type) goes supernova.

If we're doing "intelligent design", then you could probably just artificially build worlds and give them artificial, self-repairing mirrors to deflect excess heat and light to avoid the problem with red giants or excessive radiation. Perhaps insert these planets around the extra-huge habitable zones of an B or O-type star, a red giant/supergiant, etc. and see what happens with the immense radiation (even in the habitable zone) and if any extremophiles can survive a supernova up close. Or perhaps arrange the solar system in a way that would cause the habitable zone planets to migrate outward during the red giant phase to get that extra few hundred million years. Or even have life evolve in an ocean underneath an icecap outside the habitable zone, have the red giant melt the ocean, and then arrange the solar system to spiral inwards as the red giant becomes a white dwarf since if the planet is close enough. There's a lot of possibilities here.
It's not that unknown. Remember that the Moon formed much, much closer to Earth, possibly just beyond the Roche limit. At that distance (about four times the radius of Earth), the Moon would have exerted a tidal acceleration of approximately 4* 10^-3 m/s^2, which is pretty close to 4 000 times bigger than the current value. It wouldn't have dropped as low as merely ten times the current value until the Moon moved at least 25 or so Earth radii away from Earth, which would have taken somewhere between 500 million and a billion years to reach. Didn't seem to hurt the Earth that much...
It probably wasn't good for the diversity of life since all of that tidal heating would slow down the rate at which the planet cooled and prevented the formation of continents. On the other hand, a more distant moon would mean less tides and potentially not enough volcanic activity. I'm not sure if it's good or bad for life overall although if you want to avoid that issue you could just have the moon(s) captured or formed as a double planet rather than the more traumatic way our moon formed. I believe that would mean the orbit wouldn't be migrating outward as our moon is.
 
You don't need a quasar for that. If you want a good habitable zone, you'd want an F5V-F9V main sequence star which has one over 1 AU wide. They'll still live for 2-3 billion years on the main sequence (Procyon, an F5V star, for instance is about 2 billion years old and will evolve into a red giant in about 10 million years). Larger stars are more likely to form gas giants, which may be in the habitable zone. For instance, Iota Horologii (a G0V star slightly larger than the Sun) has a planet twice the size of Jupiter at around Earth's orbit. These gas giants are also more likely to be super-Jupiters or even brown dwarf companions which means Earth-size exomoons are more likely. This means you could easily pack in 2 or 3 planets in the habitable zone and maybe a few sizable worlds at the trojan points of those gas giants. Depending on the system, it's possible to have trojan planets in the size range between Mars and Earth but I don't think you'd be able to have, say, three gas giants each with a trojan planet at their L4-L5 point (for 6 trojan planets).

As for life around an F-type main sequence star, they'd be subject to higher levels of radiation from the star than Earth was which means that as long as an ozone layer developed early, there would be more incentive for life to both emerge and develop, since stellar radiation is one driver of evolution. And if you have several exomoons and trojan planets, it's very possible that abiogenesis on one world could seed much of that system with life. The 2-3 billion year "time limit" sucks, but we don't know if 4 billion years to have a "Cambrian explosion" type radiation of life is common or not. I think 1.5-2 billion years is possible for a Cambrian explosion type event. And if you want/have sentient life, evolving in a moon around a gas giant with an F-type main sequence star putting out far more energy than the Sun if you get up close is pretty much the single most optimal set-up possible.

Early F-type (F0V-F4V) or especially later A-type (A5V-A9V, like Altair) would be better in terms of every factor I mentioned above, but you're really pushing plausibility to have complex life evolve before the red giant phase (which is 1.3-2 billion years here). Although these star systems might work very well if you have life evolve in the ocean on a "snowball Earth" type moon outside the habitable zone. This would give several hundred million additional years for life to develop although there's going to be an issue with the atmosphere (not enough time for an oxygen atmosphere to develop). Early A-type stars wouldn't work without inserting already complex life onto planets and moons there, and B-type stars wouldn't work at all because the star is already a red giant by the time the planet cools from formation and anything above 8 solar masses (early B-type) goes supernova.

If we're doing "intelligent design", then you could probably just artificially build worlds and give them artificial, self-repairing mirrors to deflect excess heat and light to avoid the problem with red giants or excessive radiation. Perhaps insert these planets around the extra-huge habitable zones of an B or O-type star, a red giant/supergiant, etc. and see what happens with the immense radiation (even in the habitable zone) and if any extremophiles can survive a supernova up close. Or perhaps arrange the solar system in a way that would cause the habitable zone planets to migrate outward during the red giant phase to get that extra few hundred million years. Or even have life evolve in an ocean underneath an icecap outside the habitable zone, have the red giant melt the ocean, and then arrange the solar system to spiral inwards as the red giant becomes a white dwarf since if the planet is close enough. There's a lot of possibilities here.

It probably wasn't good for the diversity of life since all of that tidal heating would slow down the rate at which the planet cooled and prevented the formation of continents. On the other hand, a more distant moon would mean less tides and potentially not enough volcanic activity. I'm not sure if it's good or bad for life overall although if you want to avoid that issue you could just have the moon(s) captured or formed as a double planet rather than the more traumatic way our moon formed. I believe that would mean the orbit wouldn't be migrating outward as our moon is.

I do need an accretion disk. Think about it--a habitable zone measured in light-years rather than AUs automatically takes away the concern of distance limit, and the accretion disk has no deadline, unlike those dwarves and giants. And I don't get to tidally lock those planets, which would be a death sentence for any of the Earth seeds.
 
I do need an accretion disk. Think about it--a habitable zone measured in light-years rather than AUs automatically takes away the concern of distance limit, and the accretion disk has no deadline, unlike those dwarves and giants. And I don't get to tidally lock those planets, which would be a death sentence for any of the Earth seeds.
I'm sorry, what? Not being tidally locked is not a "death sentence," just look at...er...Earth.

Also, a quasar's accretion disk does have a deadline--what do you think an accretion disk is? It's material that's falling into the central supermassive black hole. Unless there's a constant supply of new material, eventually the entire accretion disk is going to be consumed or blown away by the resulting radiation. In fact the natural lifetime of quasars seems to only be comparable to late G-type stars, about 13 billion years, before they've consumed everything in range and become quiescent. And if you're doing something like creating and sustaining an artificial accretion disk over a much longer timeframe, you might as well cut the crap and build a Birchworld powered by the Penrose process instead. Much more efficient and capable of providing just as much (actually, considerably more) land and sea area than any combination of planets orbiting the black hole can.

Such a system would also be much more sustainable, too. Illuminating a surface the same area as Earth will require about 173 PW of power, which is equivalent to converting about 2 kg of matter into energy each second. The Penrose process can extract a maximum of about 29% of the starting mass-energy of an (uncharged) black hole, so since Sagittarius A* has a mass of about 8 * 10^36 kg (that is, about four million times the solar mass of 2 * 10^30 kg), it could therefore theoretically provide energy to illuminate such a world for about 10^36 years (29% of 8 * 10^36 = 2.32 * 10^36) if you extract mass-energy 100% efficiently. Such a period is 10^26 times longer than the lifespan of the Sun. Alternatively, one could extract enough energy to illuminate a million worlds simultaneously and illuminate them for a mere 10^30 years, or a hundred quintillion times longer than the lifespan of the Sun (and still a quintillion times longer than even the lifespan of a red dwarf). Either seems much more than adequate for any amount of speculative evolution you care to imagine.

EDIT: Whoops, I made a math error here. "Years" in the above should be converted into "seconds". This will reduce all of the time factors when reexpressed in years by ~10^7 (so about 10^29 years for one Earth, 10^13 years for a million). This is still much longer than the lifetime of the Sun, of course, or even than the lifetime of a red dwarf (although 10^13 years is only a few trillion years longer, not that much overall).

It probably wasn't good for the diversity of life since all of that tidal heating would slow down the rate at which the planet cooled and prevented the formation of continents. On the other hand, a more distant moon would mean less tides and potentially not enough volcanic activity. I'm not sure if it's good or bad for life overall although if you want to avoid that issue you could just have the moon(s) captured or formed as a double planet rather than the more traumatic way our moon formed. I believe that would mean the orbit wouldn't be migrating outward as our moon is.
An even bigger issue was probably the lack of oxygen in the atmosphere--there wasn't any until the Moon was about 2 billion years old (that is, about 2 and a half billion years ago), by which point the tidal forces would have been rather similar to today's (and in fact had been for a considerable period of time, as per my earlier comment). All the land in the world wouldn't matter if nothin but anaerobic microbes could live there. This is also why I think your assessment of the time frames for F-type stars is optimistic and I tend to favor G, K, or M-types for naturally occurring planets (for artificial planets and habitats, of course, these time limits can be basically side-stepped and are irrelevant). I think time is more important than any amount of radiation for the development and evolution of more complex forms.
 
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I do need an accretion disk. Think about it--a habitable zone measured in light-years rather than AUs automatically takes away the concern of distance limit, and the accretion disk has no deadline, unlike those dwarves and giants. And I don't get to tidally lock those planets, which would be a death sentence for any of the Earth seeds.
An accretion disk probably means too much meteorite bombardment. The dust and debris would cause excessive heating too I believe but the real problem is the quasar's insane radiation which is orders of magnitude higher than any star.

And I think a 1.1 AU habitable zone would be plenty sufficient. As I said, that's enough for two-three Neptune-sized (or larger) worlds with several large moons each and potentially large rocky worlds at the L4-L5 points as trojan planets.

Also, many larger stars have brown dwarf or red dwarf companions which may have their own system. Upsilon Andromedae (an F-type main sequence star) with its four super-Jupiters (one in the habitable zone, one which will be when the star evolves into a red giant) is a good example since it has a smaller red dwarf orbiting it.
An even bigger issue was probably the lack of oxygen in the atmosphere--there wasn't any until the Moon was about 2 billion years old (that is, about 2 and a half billion years ago), by which point the tidal forces would have been rather similar to today's (and in fact had been for a considerable period of time, as per my earlier comment). All the land in the world wouldn't matter if nothin but anaerobic microbes could live there. This is also why I think your assessment of the time frames for F-type stars is optimistic and I tend to favor G, K, or M-types for naturally occurring planets (for artificial planets and habitats, of course, these time limits can be basically side-stepped and are irrelevant). I think time is more important than any amount of radiation for the development and evolution of more complex forms.
Oxygen Crisis is definitely a problem but that's one of those events that's hard to put a timeframe on. My thought was there could be faster evolution of photosynthesizing bacteria thanks to the greater radiation meaning the atmosphere becomes oxygen faster. A larger star with more radiation also burns away atmospheric methane more efficiently. The star wouldn't be the only factor though, you'd need lower metallicity in the star system in general so the planet forms with less iron to act as an oxygen sink. This could mean life was more common around F-type stars billions of years ago when metallicity was lower so red giant and white dwarf systems might have a lot of life underneath the ice.

And while a star like Procyon might only live 2 billion years before the red giant phase, on the smaller end you do have the aforementioned Upsilon Andromedae which is 3.2 billion years old and tens of millions of years left on the main sequence.

I think the relative rarity of F-type stars (and early G-type stars like Eta Cassiopeiae) is a large part of why we don't see evidence of sentient civilizations born in a setting like this which would be more likely if we assume faster radiation of life is possible. It might also be true that exomoons would tend toward being water worlds and thus ill-suited for technologically advanced life. You're definitely right about the fact time is the most important factor, but in the early universe larger stars (G/F stars) could be more likely to have complex life.

Of course if you're playing intelligent design like the post I replied to then you don't have to worry about that particular hurdle and can seed the planets with cyanobacteria as well as eukaryotic/primitive multicellular life.
 
Absolutely. Make sure that they're outside each other's Roche limit (20 000 km is a good minimum distance, but probably further), but well within their Hill sphere (don't go further than 1 000 000 km). They'll likely be tidally locked; if they're close enough to each other, this means noon eclipses every day in the inner hemispheres. Around 50 000 km radius will get you a slightly shorter than Earth-length day, assuming they're tidally locked.
 
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