Frost line (astrophysics)

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In astronomy or planetary science, the frost line, also known as the snow line or ice line, is the minimum distance from the central protostar of a solar nebula where the temperature is low enough for volatile compounds such as water, ammonia, methane, carbon dioxide and carbon monoxide to condense into solid grains, which will allow their accretion into planetesimals. Beyond the line, otherwise gaseous compounds (which are much more abundant) can be quite easily condensed to allow formation of gas and ice giants; while within it, only heavier compounds can be accreted to form the typically much smaller rocky planets.

Contents

The term itself is borrowed from the notion of "frost line" in soil science, which describes the maximum depth from the surface that groundwater can freeze.

Each volatile substance has its own frost line (e.g. carbon monoxide, [1] nitrogen, [2] and argon [3] ), so it is important to always specify which material's frost line is referred. A tracer gas may be used for materials that are otherwise difficult to detect; for example diazenylium for carbon monoxide.

Location

Different volatile compounds have different condensation temperatures at different partial pressures (thus different densities) in the protostar nebula, so their respective frost lines will differ. The actual temperature and distance for the snow line of water ice depend on the physical model used to calculate it and on the theoretical solar nebula model:

The location of the frost line changes over time, potentially reaching a maximum radius of 17.4 AU for a solar-mass star before decreasing thereafter. [8]

Current snow line versus formation snow line

The radial position of the condensation/evaporation front varies over time, as the nebula evolves. Occasionally, the term snow line is also used to represent the present distance at which water ice can be stable (even under direct sunlight). This current snow line distance is different from the formation snow line distance during the formation of the Solar System, and approximately equals 5 AU. [9] The reason for the difference is that during the formation of the Solar System, the solar nebula was an opaque cloud where temperatures were lower close to the Sun,[ citation needed ] and the Sun itself was less energetic. After formation, the ice got buried by infalling dust and it has remained stable a few meters below the surface. If ice within 5 AU is exposed, e.g. by a crater, then it sublimates on short timescales. However, out of direct sunlight ice can remain stable on the surface of asteroids (and the Moon and Mercury) if it is located in permanently shadowed polar craters, where temperature may remain very low over the age of the Solar System (e.g. 30–40 K on the Moon).

Observations of the asteroid belt, located between Mars and Jupiter, suggest that the water snow line during formation of the Solar System was located within this region. The outer asteroids are icy C-class objects (e.g. Abe et al. 2000; Morbidelli et al. 2000) whereas the inner asteroid belt is largely devoid of water. This implies that when planetesimal formation occurred the snow line was located at around 2.7 AU from the Sun. [6]

For example, the dwarf planet Ceres with semi-major axis of 2.77 AU lies almost exactly on the lower estimation for water snow line during the formation of the Solar System. Ceres appears to have an icy mantle and may even have a water ocean below the surface. [10] [11]

Planet formation

The lower temperature in the nebula beyond the frost line makes many more solid grains available for accretion into planetesimals and eventually planets. The frost line therefore separates terrestrial planets from giant planets in the Solar System. [12] However, giant planets have been found inside the frost line around several other stars (so-called hot Jupiters). They are thought to have formed outside the frost line, and later migrated inwards to their current positions. [13] [14] Earth, which lies less than a quarter of the distance to the frost line but is not a giant planet, has adequate gravitation for keeping methane, ammonia, and water vapor from escaping it. Methane and ammonia are rare in the Earth's atmosphere only because of their instability in an oxygen-rich atmosphere that results from life forms (largely green plants) whose biochemistry suggests plentiful methane and ammonia at one time, but of course liquid water and ice, which are chemically stable in such an atmosphere, form much of the surface of Earth.

Researchers Rebecca Martin and Mario Livio have proposed that asteroid belts may tend to form in the vicinity of the frost line, due to nearby giant planets disrupting planet formation inside their orbit. By analysing the temperature of warm dust found around some 90 stars, they concluded that the dust (and therefore possible asteroid belts) was typically found close to the frost line. [15] The underlying mechanism may be the thermal instability of snow line on the timescales of 1,000 - 10,000 years, resulting in periodic deposition of dust material in relatively narrow circumstellar rings. [16]

See also

Related Research Articles

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<span class="mw-page-title-main">Terrestrial planet</span> Planet that is composed primarily of silicate rocks or metals

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<span class="mw-page-title-main">Planetesimal</span> Solid objects in protoplanetary disks and debris disks

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<span class="mw-page-title-main">Nebular hypothesis</span> Astronomical theory about the Solar System

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<span class="mw-page-title-main">Ocean world</span> Planet containing a significant amount of water or other liquid

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<span class="mw-page-title-main">HD 113766</span> Binary star in the constellation Centaurus

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<span class="mw-page-title-main">Nice model</span> Scenario for the dynamical evolution of the Solar System

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<span class="mw-page-title-main">Circumstellar disc</span> Accumulation of matter around a star

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<span class="mw-page-title-main">Pebble accretion</span>

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In planetary science a streaming instability is a hypothetical mechanism for the formation of planetesimals in which the drag felt by solid particles orbiting in a gas disk leads to their spontaneous concentration into clumps which can gravitationally collapse. Small initial clumps increase the orbital velocity of the gas, slowing radial drift locally, leading to their growth as they are joined by faster drifting isolated particles. Massive filaments form that reach densities sufficient for the gravitational collapse into planetesimals the size of large asteroids, bypassing a number of barriers to the traditional formation mechanisms. The formation of streaming instabilities requires solids that are moderately coupled to the gas and a local solid to gas ratio of one or greater. The growth of solids large enough to become moderately coupled to the gas is more likely outside the ice line and in regions with limited turbulence. An initial concentration of solids with respect to the gas is necessary to suppress turbulence sufficiently to allow the solid to gas ratio to reach greater than one at the mid-plane. A wide variety of mechanisms to selectively remove gas or to concentrate solids have been proposed. In the inner Solar System the formation of streaming instabilities requires a greater initial concentration of solids or the growth of solid beyond the size of chondrules.

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References

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  2. ↑ Dartois, E.; Engrand, C.; Brunetto, R.; Duprat, J.; Pino, T.; Quirico, E.; Remusat, L.; Bardin, N.; Briani, G.; Mostefaoui, S.; Morinaud, G.; Crane, B.; Szwec, N.; Delauche, L.; Jamme, F.; Sandt, Ch.; Dumas, P. (2013). "UltraCarbonaceous Antarctic micrometeorites, probing the Solar System beyond the nitrogen snow-line by E. Dartois, et al". Icarus. 224 (1): 243–252. Bibcode:2013Icar..224..243D. doi:10.1016/j.icarus.2013.03.002.
  3. ↑ Öberg, K.I.; Wordsworth, R. (2019). "Jupiter's Composition Suggests its Core Assembled Exterior to the N_{2} Snowline". The Astronomical Journal. 158 (5). arXiv: 1909.11246 . doi: 10.3847/1538-3881/ab46a8 . S2CID   202749962.
  4. ↑ "Structure of the Solar Nebula, Growth and Decay of Magnetic Fields and Effects of Magnetic and Turbulent Viscosities on the Nebula by Chushiro Hayashi". Archived from the original on 2015-02-19.
  5. ↑ Podolak, M.; Zucker, S. (2004). "A note on the snow line in protostellar accretion disks by M. PODOLAK and S. ZUCKER, 2010". Meteoritics & Planetary Science. 39 (11): 1859. Bibcode:2004M&PS...39.1859P. doi: 10.1111/j.1945-5100.2004.tb00081.x . S2CID   55193644.
  6. 1 2 Martin, Rebecca G.; Livio, Mario (2012). "On the Evolution of the Snow Line in Protoplanetary Discs by Rebecca G. Martin, Mario Livio (STScI)". Monthly Notices of the Royal Astronomical Society: Letters. 425 (1): L6. arXiv: 1207.4284 . Bibcode:2012MNRAS.425L...6M. doi:10.1111/j.1745-3933.2012.01290.x. S2CID   54691025.
  7. ↑ D'Angelo, G.; Podolak, M. (2015). "Capture and Evolution of Planetesimals in Circumjovian Disks". The Astrophysical Journal. 806 (1): 29pp. arXiv: 1504.04364 . Bibcode:2015ApJ...806..203D. doi:10.1088/0004-637X/806/2/203. S2CID   119216797.
  8. ↑ Zhang, Yu; Jin, Liping (March 2015). "The Evolution of the Snow Line in a Protoplanetary Disk". The Astrophysical Journal. 802 (1). id. 58. Bibcode:2015ApJ...802...58Z. doi:10.1088/0004-637X/802/1/58.
  9. ↑ Jewitt, D.; Chizmadia, L.; Grimm, R.; Prialnik, D. (2007). "Water in the Small Bodies of the Solar System" (PDF). In Reipurth, B.; Jewitt, D.; Keil, K. (eds.). Protostars and Planets V. University of Arizona Press. pp. 863–878. ISBN   978-0-8165-2654-3.
  10. ↑ McCord, T. B.; Sotin, C. (2005-05-21). "Ceres: Evolution and current state". Journal of Geophysical Research: Planets. 110 (E5): E05009. Bibcode:2005JGRE..110.5009M. doi: 10.1029/2004JE002244 .
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  14. ↑ D'Angelo, Gennaro; Durisen, Richard H.; Lissauer, Jack J. (December 2010). "Giant Planet Formation". In Seager, Sara (ed.). Exoplanets. University of Arizona Press. pp. 319–346. arXiv: 1006.5486 . Bibcode:2010exop.book..319D. ISBN   978-0-8165-2945-2.
  15. ↑ "Asteroid Belts of Just the Right Size are Friendly to Life". NASA. 1 November 2012. Retrieved 3 November 2012.
  16. ↑ Owen, James E. (2020). "Snow-lines can be thermally unstable". Monthly Notices of the Royal Astronomical Society. 495 (3): 3160–3174. arXiv: 2005.03665 . doi:10.1093/mnras/staa1309.
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