2013
Exomoon Habitability Constrained by Illumination and Tidal Heating
Abstract: The detection of moons orbiting extrasolar planets (''exomoons'') has now become feasible. Once they are discovered in the circumstellar habitable zone, questions about their habitability will emerge. Exomoons are likely to be tidally locked to their planet and hence experience days much shorter than their orbital period around the star and have seasons, all of which works in favor of habitability. These satellites can receive more illumination per area than their host planets, as the planet reflects stellar l…
View preprint versions
Search citation statements
Paper Sections
Select...
123
47
11
2
Citation Types
2
199
0
1
Year Published
2005
2026
Publication Types
Select...
112
28
20
1
Relationship
17
144
Authors
Journals
Cited by 159 publications
(202 citation statements)
References 152 publications
2
199
0
1
“…However, in this instance we have placed the planet near the Hill radius, r H = 0.022 AU, where a pm = 0.02 AU. For this system, the orbit of the moon dominates the flux profile such that P pm /P sp = 1/10, which is within the bound determined by Kipping (2009) and Heller & Barnes (2013). The average total flux fluctuation, ∼ 43.07 W/m 2 , is smaller in this example system compared to the same system at various planetary eccentricities, most likely as a result of the larger a pm .…”
Section: Hill Radius Vs Tidal Locking Radiussupporting
confidence: 73%
“…However, in this instance we have placed the planet near the Hill radius, r H = 0.022 AU, where a pm = 0.02 AU. For this system, the orbit of the moon dominates the flux profile such that P pm /P sp = 1/10, which is within the bound determined by Kipping (2009) and Heller & Barnes (2013). The average total flux fluctuation, ∼ 43.07 W/m 2 , is smaller in this example system compared to the same system at various planetary eccentricities, most likely as a result of the larger a pm .…”
Section: Hill Radius Vs Tidal Locking Radiussupporting
confidence: 73%
“…Hence, the snow line can be regarded as a circumstellar subsurface habitable edge. Like Heller & Barnes (2013), we also find a circumplanetary habitable edge, although we believe (at least when it concerns subsurface habitability) it better regarded as a maximum melting criterion because it depends on multiple parameters. Regardless, we speculate that subsurface habitable exomoons may populate the parameter space from the least massive rounded moons (Mimas and Enceladus) to at least Titania, and possibly well beyond.…”
Section: Discussionsupporting
confidence: 54%
“…We hypothesize that the circumstellar subsurface habitable zone for exomoons, similar to its surface counterpart, extends farther out than for planets because of additional heating by the planet and tidal effects. In addition, we hope to find a circumplanetary subsurface habitable edge similar to the one described by Heller & Barnes (2013) for surface habitability.…”
Section: Introductionmentioning
confidence: 67%
“…The four different categories of candidates allow the reader to adopt the criteria that are most useful for a particular followup program. For example, giant planets in the optimistic HZ (Table 4) may be useful for those interesting in HZ exomoons where a wider range of incident flux can account for additional energy sources from tidal energy, etc (Heller & Barnes 2013;Hinkel & Kane 2013). Our analysis of the radii distributions for candidates in the HZ compared with the general candidate population shows that the two are very similar within the constraints of selection effects and systematic noise that impacts longer-period terrestrial planets.…”
Section: Discussionmentioning
confidence: 68%
