3 ms·
This article by Lhotka & Gale (2019) <https://arxiv.org/abs/1911.02778 https://arxiv.org/abs/1911.02778> is a little beyond my patience for understanding, but t
by zyrxvo 4y ago
This article by Lhotka & Gale (2019) <https://arxiv.org/abs/1911.02778 https://arxiv.org/abs/1911.02778> is a little beyond my patience for understanding, but they have an excellent parameter space plot in Figure 1 relating a bunch of different effects with respect to dust grain size. Their figure only goes up to grains 1 cm in size though. However, it's a detailed paper on the relative "importance of the interplanetary magnetic field on the orbital evolution of dust". I met Lhotka at a conference where they presented this work.
I think this discussion is really fascinating, and it's certainly something that I didn't consider when working on the paper. However, I think the results that we found can be generalized to better understand how a small effect might impact the stability of the solar system on a statistical level, even if we can't say much about the effect in specific cases.
For example, I expect that as the total mass of the sun decreases due to solar wind the secular frequencies would all change by the same amount, proportional to the decrease in mass <https://arxiv.org/abs/1811.07135 https://arxiv.org/abs/1811.07135>. This would mean that the difference between the g1 and g5 modes would be closer by the same amount. However, we wouldn't expect the secular diffusion to change so it would be more akin to dashed line in Figure 2 of our paper. So stellar mass loss could cause Mercury to go unstable sooner than without mass loss, but we wouldn't expect the effect to be significant.
- raattgift 4y ago"In the planetary system, solar gravity determines the orbits of all bodies larger than dust particles for which other forces become important. But even for dust, gravity is an important factor. Near planets, planetary gravity takes over", §3.1 of Krüger & Grün's Chapter 29 in Encyclopedia of the Solar System (2014) <https://doi.org/10.1016/B978-0-12-415845-0.00029-3 https://doi.org/10.1016/B978-0-12-415845-0.00029-3> (it's on scy hob :) ). See Table 29.4. Where dust is gravitationally interesting at the present age of the solar system is probably in ring/moon interactions, but mostly with the moon acting on the ring dusts as with Saturn's Daphnis and Pan (Cassini). Of course there was a lot more dust doing a lot more interesting things gravitationally much earlier in the solar system's history, which might be interesting if you decide to use your approach to simulate the solar system's past (some of that dust could be related to your link to the massive early sun hypothesis paper). :-) Your other paper on stellar flybys provokes an interesting question: could a fly-by deposit a significant mass of trans-Neptunian dust? I'd wager a lot of fresh dust captured out there could increase the eccentricity of planetary orbits through your 0.9 threshold. Although not plausible for the solar system, relatively high mass-density dust around compact binaries can drive the compact binary's orbital evolution. See for example the very fresh Siwek, Weinberger & Hernquist (2023) <https://arxiv.org/abs/2302.01785 https://arxiv.org/abs/2302.01785>, reasonably summarized at <https://astrobites.org/2023/03/13/will-it-merge-investigating-how-gas-disks-can-determine-the-future-of-a-binary-black-hole-system/ https://astrobites.org/2023/03/13/will-it-merge-investigatin...>.