The enigmatic ‘Oumuamua continues to stir controversy. Last week we looked at a new paper from Jennifer Bergner (UC-Berkeley) and Darryl Seligman (Cornell University), discussing a mechanism for the interstellar object’s unusual non-gravitational acceleration. The researchers explored the possibility that ice impacted by high-energy particles like cosmic rays would dissociate water in a comet to create molecular hydrogen within the ice. Was the warming of this hydrogen, all but undetectable according to the authors, the cause of outgassing and the anomalous acceleration?

Image: This very deep combined image shows the interstellar object ‘Oumuamua at the center of the image. It is surrounded by the trails of faint stars that are smeared as the telescopes tracked the moving comet. Credit: ESO/K. Meech et al.

Answering the question in a paper just submitted to the arXiv site is Harvard’s Avi Loeb, working with Thiem Hoang (Korea University of Science and Technology), who home in on Bergner and Seligman’s finding that the surface temperature of ‘Oumuamua can exceed 140 K at perihelion, enough to produce this evaporation. Loeb and Hoang argue that this calculation ignores the effect of evaporative cooling of the molecular hydrogen. The authors proceed to take such cooling into account and find that the surface temperature of H2 water ice is lower than that calculated by Bergner and Seligman by a factor of 9. This is turn reduces the projected outgassing.

From the paper:

…we found that the evaporative cooling is much more efficient than radiative cooling at temperatures above 20 K (see Figure 1, left panel). By taking into account the evaporative cooling by H2 evaporation, our results (see Figure 1, right panel) show that the surface temperatures of H2-water ice are lower by a factor of 9 than the temperature obtained by Bergner & Seligman (2023) (see their figure 3). Therefore, the thermal speed of outgassing H2 is decreased by a factor of 3.

Image: This is Figure 1 from the paper. Caption: Left panel: comparison of heating and cooling rates when the object is located at 1.4 times the Earth separation from the sun. Evaporative cooling by H2 is dominant over radiative cooling. The intersection of heating and total cooling determines the equilibrium surface temperature. Right panel: surface temperature at different distances, calculated for the case with (solid lines) and without (dashed-dotted line) evaporative cooling. Different ratio of H2 to water is assumed. Evaporative cooling by H2 decreases significantly the surface temperature compared to the case without evaporative cooling (dashed-dotted line).

And this is a problem for the molecular hydrogen evaporation scenario. The result of this decrease in outgassing is that ‘Oumuamua would have had to have been what the authors call an ‘oxygen iceberg’ to produce enough molecular hydrogen to drive the observed acceleration, a highly unlikely scenario for the following reason:

Given this constraint, the requirement for a surface layer that is made of pure molecular hydrogen will not survive the journey through interstellar space as a result of heating by starlight (Hoang & Loeb 2020). Moreover, the lower surface temperature also influences the thermal annealing of water ice, a key process that is appealed to by Bergner & Seligman (2023) to release H2.

The paper is Hoang & Loeb, “Implications of evaporative cooling by H2 for 1I/‘Oumuamua” (full text).

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