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Let's suppose a solar system:

  • A main-sequence star similar to the Sun. G2V or so.
  • A Hot/Warm Jupiter HJ with a semi-major axis somewhere from 0.5 AU to 0.0001 AU.
  • An Earth-like planet EL with a semi-major axis somewhere around 1 AU, with a magnetosphere, composition, water amount comparable to Earth. Life/civilization should exist in some fashion, though exact technology level is unknown.
  • The angles of inclinations of their orbits are a couple of degrees apart.

According to this and a multitude of other sources, Hot Jupiters tend to be losing their atmosphere due to their proximity to their sun. Similar to a comet tail, I would expect that atmosphere to be pushed out from HJ by the solar wind; it would probably also disperse some with distance.

  • Would this dispersed atmosphere from the HJ have any effect on the EL?
  • If there is an effect, where along EL's orbit is there an effect? Would it happen along all of the orbit, because of the dispersal? Would it happen only when the EL crosses a transit node? Or only when there's a transit (or when the EL passes through the transit node a couple of days after the HJ does, since it takes time for the atmosphere particles to get from one orbit to the other)
  • Would the dispersed atmosphere in space even be visible from EL, or is it likely just too thin?
  • If the dispersed atmosphere has an effect on the EL, would that have any impact on life on EL? Technology e.g. radios?

(Though this question is tagged [science-based], citations/math would be awesome)

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  • $\begingroup$ I can't really contribute to the question but I would like to point out that having a gas giant at such close quarters does not bear well for the stability of the Earth-like planet's orbit in the short term, never mind the atmospheric loss. $\endgroup$ – pablodf76 Apr 25 '17 at 21:00
  • $\begingroup$ A fair point, though that's also on my list to run some simulations of. I've sometimes been surprised at what ends up being stable. For now, let's assume the masses and distances are such that we have a reasonably stable system, at least for a couple thousand years. $\endgroup$ – Keith B Apr 25 '17 at 21:05
  • $\begingroup$ Having run some simulations in Rebound with a Jupiter mass at about 0.5 AU and an Earth mass at about 1 AU, the system appears reasonably stable, though the EL's inclination varies over the course of thousands of years, pulled by the HJ. This is stable enough for colonization, at least. $\endgroup$ – Keith B Apr 26 '17 at 4:08
  • $\begingroup$ What is the rate of mass loss from the hot Jupiter? That would make a big difference. $\endgroup$ – cometaryorbit Apr 30 '17 at 1:35
  • $\begingroup$ @cometaryorbit Per the linked paper's abstract, "We constrain the escape rate of atomic hydrogen to be between 10^9 and 10^{11} g/s" $\endgroup$ – Keith B May 2 '17 at 3:32
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As you've stated, the paper you cited gives the rate of atmospheric mass loss as approximately $\dot{M}=10^9\text{-}10^{11}\text{ g/s}=10^{6}\text{-}10^8\text{ kg/s}$ of hydrogen. We can convert this to mass flux as $$F_m(r)=\frac{\dot{M}}{2\pi r^2}$$ a distance $r$ from the Hot Jupiter because the atmospheric loss will not be isotropic, but only away from the star (otherwise, the denominator would be $4\pi r^2$).1 Note, though, that this could be much lower if the star is between the hot Jupiter and the Earth-like planet.

Assume that the hot Jupiter's orbit is at the far end of your range, $\sim0.5\text{ AU}$. Then, at closest approach, it could be $1\text{ AU}-0.5\text{ AU}=0.5\text{ AU}$ from the Earth-like planet, a distance of $7.48\times10^{10}\text{ m}$. Therefore, we find the flux at $0.5\text{ AU}$ to be $$F_m(0.5\text{ AU})=\frac{10^6\text{-}10^8\text{ kg/s}}{2\pi (7.48\times10^{10}\text{ m})^2}=7.1\times10^{-16}\text{-}7.1\times10^{-18}\text{ kg s}^{-1}\text{ m}^{-2}$$ The radius of this planet is about that of Earth, $6.37\times10^6\text{ m}$. Therefore, the surface area of Earth facing the hot Jupiter at closest approach is $$A=\frac{1}{2}\text{Surface Area}=\frac{1}{2}4\pi R_{\oplus}^2=2.55\times10^{14}\text{ m}^2$$ This means that, at closest approach, the mass Earth could change in mass approximately $$\dot{M}_{\oplus}=F_m(0.5\text{ AU})\times A=1.81\times10^{-3}\text{-}1.81\times10^{-1}\text{ kg/s}\simeq1\text{-}100\text{ g/s}$$ That's not insignificant, but beware: This is only applicable when the hot Jupiter is very close to the Earth-like planet, and it assumes that the hot Jupiter has a very large semi-major axis. It is much more likely that the flux will be smaller.

In short, the flux is probably going to be very small, even at the closest approach between the two planets.


A footnote on geometry

1 So, that expression is a little inaccurate. In reality, the geometry of the expelled mass will look like something of a plume, shaped by hydrodynamic and gravitational forces. Gliese 436b, an extreme case, is suffering from high mass-loss rates that cause a cloud of hydrogen to be blown away. Ehrenreich et al. (2015) modeled the system in detail:

enter image description here
Figure 3, Ehrenreich et al. (2015).

enter image description here
Figure 4, Ehrenreich et al. (2015).

This should indeed change the flux, though probably not by a substantial amount; it falls off fairly quickly. I think my original order-of-magnitude estimates are valid.

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    $\begingroup$ What effect would there be on the radiation belts around said earthlike planet? $\endgroup$ – Joe Kissling May 3 '17 at 18:49
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    $\begingroup$ @JoeKissling I'm not sure. I'd guess it would depend on the strength of the stellar wind. $\endgroup$ – HDE 226868 May 3 '17 at 19:01

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