Typical Quotes Showing How Planetary Scientists Are Currently Using the Planet Concept, 1955 – Present
In each case the authors chose to use planet instead of satellite (or dwarf planet for Ceres and Pluto) knowing that such usage would be contrary to the popular cultural terminology and/or contrary to the IAU’s definition. This usage indicates that the authors associate the planet concept with complex geophysics.
Examples for Pluto since 2008 (well after the IAU vote)
| 2008 | Hicks, M.D., Buratti, B.J., Gillam, S.D., Young, J.W. and Somers, J.F., 2008, September. Support Observations For New Horizons: Pluto’s Solar Phase Curve As Measured By The Cassini Spacecraft And A New Ground-based Optical Lightcurve. In Bulletin of the American Astronomical Society(Vol. 40, p. 460). | “… In order to constrain potential volatile transport on the surface of Pluto due to changing solarillumination geometry and heliocentric distance, we have recently measured (2007 October-2008 March) a Bessel R-band rotational lightcurve of the planet at TMO which exhibits a …” |
| 2008 | Miller, J.K., Carranza, E., Stanbridge, D. and Williams, B.G., 2008, February. New Horizons Navigation to Pluto. In AAS Guidance and Control Conference. | “Pluto/Charon/Hydra reduced optical imaging – sensitivity to planet ephemeris errors” |
| 2009 | Delamere, P.A., 2009. Hybrid code simulations of the solar wind interaction with Pluto. Journal of Geophysical Research: Space Physics, 114(A3). | “Without an escaping atmosphere, the size of Pluto’s obstacle to the solar wind (ie, planet + atmosphere), would be comparable to the upstream ion inertial length…” |
| 2009 | Kalinicheva, O. V., and V. P. Tomanov. “On the absence of an interrelation between cometary orbits and Pluto.” Solar System Research 43.6 (2009): 500-503. | “However, the closeness of the orbits of the comets and that of Pluto is insufficient for proving the connection between the comets and the planet. Even if the orbits cross, this does not mean that the comet and the planet will simultaneously end up in the cross point.” |
| 2009 | McComas, D., Allegrini, F., Bagenal, F., Casey, P., Delamere, P., Demkee, D., Dunn, G., Elliott, H., Hanley, J., Johnson, K. and Langle, J., 2009. The solar wind around Pluto (SWAP) instrument aboard New Horizons. In New Horizons (pp. 261-313). Springer New York. | “… Pluto’s thick atmosphere escapes the planet’sweak gravity and streams away as neutral particles. … Pluto represents a possible intermediate case if the interaction region is limited to an area close to the planet since the solar wind proton inertial length is roughly 2 RP.” |
| 2009 | Rannou, P. and Durry, G., 2009. Extinction layer detected by the 2003 star occultation on Pluto. Journal of Geophysical Research: Planets, 114(E11). | “In this work, as in most of the publications concerning Pluto, we will refer to the altitude levelstaken from the center of the planet since the real radius of the solid body is not well defined.” |
| 2009 | Rubincam, D.P., 2009, May. Pluto Insolation and the South Polar Cap. In AGU Spring Meeting Abstracts (Vol. 1, p. 04). | “Pluto’s south polar cap is a puzzle. The planet’s southern cap may be brighter than the north, even though it was the south pole which faced the Sun on Pluto’s recent approach to perihelion.” |
| 2009 | Sicardy, B., Boissel, Y., Colas, F., Doressoundiram, A., Lecacheux, J., Roques, F., Widemann, T., Beisker, W., Andrei, A.H., Camargo, J.I.B. and Martins, R.V., 2009, September. Constraints on Charon’s orbit from the stellar occultation of 22 June 2008. In European Planetary Science Congress 2009 (Vol. 1, p. 164). | ” fit to the five Pluto occultation light curves ob- tained in Australia,using a ray tracing method and a standard atmospheric model for the planet, provides – amongothers – Pluto’s offset with respect to it ex- pected DE413 ephemeris position.” |
| 2010 | Assafin, M., Camargo, J.I.B., Martins, R.V., Andrei, A.H., Sicardy, B., Young, L., da Silva Neto, D.N. and Braga-Ribas, F., 2010. Precise predictions of stellar occultations by Pluto, Charon, Nix, and Hydra for 2008–2015. Astronomy & Astrophysics, 515, p.A32. | “Recall that our formula for insolation doesn’t depend on the precession angle. Note that the longitude of perihelion is determined by the precession angle (as the planet precesses, its line of equinoxes changes), so our results don’t depend on the longitude of perihelion. One area of concern could be that Pluto’speriod of precession is in resonance with its orbital period. Dobrovolskis et al. show that the angle between Pluto’s perihelion and its vernal equinox have a period of about three million Earth years, or about 12,000 Pluto years [8]. Although this period is slightly faster than Earth’s precession, it is large enough so that Pluto’s precession is negligible in a Pluto year. Thus, we should have no influence from the precession angle (or longitude of precession) in the calculations of Pluto’s insolation. “It is important to note that because the mean annual insolation is symmetric across the equator, we have that any multi-year average must also be symmetric about the planet’s equator.” |
| 2010 | Roe, H., 2010. Climate change and haze on Pluto. Keck Observatory Archive NIRSPEC N150NS, 1, p.295. | “Further, these observations are important toward our long term understanding of Pluto’s changing climate as the planet recedes from perihelion…” |
| 2011 | Rawal, J.J. and Nikouravan, B., 2011. Are there rings around Pluto?. International Journal of Fundamental Physical Sciences (IJFPS), Vol. 1, No. 1, p. 6-10, 1, pp.6-10. | “Here, it is shown that a stable ring system consisting of small rocks having densities in the range (1–2.4) g cm-3 and diameters in the range (20–90) km along with fine dust and particles disrupted off these rocks, may exist around Pluto within the distance ~2500 km from the centre of the planet.” |
| 2012 | Young, Leslie A. “Volatile transport on inhomogeneous surfaces: I–Analytic expressions, with application to Pluto’s day.” Icarus 221.1 (2012): 80-88. | “This model, like that of HP96, assumes that the volatile ice temperature is the same everywhere on the planet.” |
| 2013 | Mousis, Olivier, et al. “On the possible noble gas deficiency of Pluto’s atmosphere.” Icarus 225.1 (2013): 856-861. | “The formation on Pluto of clathrates rich in noble gases could then induce a strong decrease in their atmospheric abundances relative to their initial values. A clathrate thickness of order of a few centimeters globally averaged on the planet is enough to …” |
| 2013 | STERN, A. and SPENCER, J., 2013. ‘Southwest Research Institute, Department of Space Studies, 1050 Walnut Street, Suite 400. The First Decadal Review of the Edgeworth-Kuiper Belt, p.477. | “The trans-Neptunian region, containing the binary planet Pluto–Charon and the myriad planetary embryos of the Kuiper Belt, is a scientific and intellectual frontier” |
| 2013 | Zalucha, Angela M., and Timothy I. Michaels. “A 3D general circulation model for Pluto and Triton with fixed volatile abundance and simplified surface forcing.” Icarus 223, no. 2 (2013): 819-831. | “This is unique versus other planetary atmospheresin the Solar System, such as Earth, Venus, Mars, Titan, and the giant planets. These planets have one or more overturning circulation patterns such as Hadley, Walker, or eddy driven circulations.” and “Fig. 12 shows a zonally and time averaged latitude-height temperature cross-section for Pluto…Fig. 13 shows the corresponding zonally and time averaged latitude-height cross section of mass stream function… at solstice there is a single planet-wide cell.” |
| 2014 | Cruikshank, D.P., Pinilla-Alonso, N. and Binzel, R.P., 2014. Rotationally resolved spectrum of Pluto, ices and non-ice surface constituents. NOAO Proposal, 1, p.272. | “We propose to obtain the first ever high-precision spectra of Plutoin the region 0.3 to 0.9 nm at several disk-averaged positions on the planet’s surface.” |
| 2014 | Kratter, K.M. and Shannon, A., 2014. Planet packing in circumbinary systems. Monthly Notices of the Royal Astronomical Society, 437(4), pp.3727-3735. | “The Pluto–Charon planet–satellite system consists of a binary orbited by four low-mass satellites.” |
| 2014 | Nakajima, M., Genda, H., Asphaug, E. and Ida, S., 2014, November. Constraints on Exomoon Formation. In AAS/Division for Planetary Sciences Meeting Abstracts(Vol. 46). | “This upper limit is a few Earth masses for a rocky planet, and about an Earth mass for an icy planet. These results are consistent with the models that Earth’s and Pluto’s satellites formed by impacts.” |
| 2014 | Showalter MR. Chaotic Rotation of Nix and Hydra. InAAS/Division of Dynamical Astronomy Meeting 2014 May (Vol. 45). | “… the mystery, Nix increased in absolute brightness by about 30% between 2010 and 2012, whereasHydra was stable.I have developed a numeric integrator that tracks the position, velocity,orientation and rotation state of a moon as it orbits the Pluto-Charon “binary planet“. …However, both photometry and dynamical simulations support the notion that chaotic rotation is a natural state for irregularly-shaped bodies orbiting a binary planet, with Nix and Hydra as real-world examples.” |
| 2015 | Bagenal, F., Delamere, P.A., Elliott, H.A., Hill, M.E., Lisse, C.M., McComas, D.J., McNutt Jr, R.L., Richardson, J.D., Smith, C.W. and Strobel, D.F., 2015. Solar wind at 33 AU: Setting bounds on the Pluto interaction for New Horizons. Journal of Geophysical Research: Planets, 120(9), pp.1497-1511. and Bagenal, F., Delamere, P.A., Elliott, H.A., Hill, M.E., Lisse, C.M., McComas, D.J., McNutt Jr, R.L., Richardson, J.D., Smith, C.W. and Strobel, D.F., 2015, December. Solar Wind at 33 AU: Setting Bounds on the Pluto Interaction. In AGU Fall Meeting Abstracts. | “Pluto has a tenuous, extended atmosphere that is escaping the planet’s weak gravity.” |
| 2015 | Correia, A.C., Leleu, A., Rambaux, N. and Robutel, P., 2015. Spin-orbit coupling and chaotic rotation for circumbinary bodies-Application to the small satellites of the Pluto-Charon system. Astronomy & Astrophysics, 580, p.L14. | “…Charon has an important fraction of the total mass (about 11%), and therefore the system is considered a binary planet rather than a planet and a moon.” |
| 2015 | Cruikshank, D.P., Grundy, W.M., Stern, S.A., Olkin, C.B., Cook, J.C., Dalle Ore, C.M., Binzel, R.P., Earle, A.M., Ennico, K., Jennings, D.E. and Howett, C.J., 2015, November. Pluto: Distribution of ices and coloring agents from New Horizons LEISA observations. In AAS/Division for Planetary Sciences Meeting Abstracts(Vol. 47). | “… laboratory by energetic processing of mixtures of the ices (N 2 , CH 4 , CO) known on Pluto’s surface. We present results returned from the spacecraft to date obtained from the analysis of the high spatial resolution dataset obtained near the time of closest approach to the planet. …” |
| 2015 | Cruikshank, D.P., Imanaka, H., Dalle Ore, C., Sandford, S.A. and Nuevo, M., 2015, December. Tholins as Coloring Agents on Pluto. In AGU Fall Meeting Abstracts. | “The shape of the reflectance spectrum of Plutorecorded with telescopes, 0.3-1.0 mum, shows the planet’s yellow-red color (1).” |
| 2015 | Hamilton, D.P., 2015, December. The Cold and Icy Heart of Pluto. In AGU Fall Meeting Abstracts. | “We find that the annual average insolation is always symmetric about Pluto’sequator and is fully independent of the relative locations of the planet’s pericenter and equinoxes.” |
| 2015 | Jacobson, R.A., Brozovic, M., Buie, M., Porter, S., Showalter, M., Spencer, J., Stern, S.A., Weaver, H., Young, L., Ennico, K. and Olkin, C., 2015, November. The Orbits and Masses of Pluto’s Satellites after New Horizons. In AAS/Division for Planetary Sciences Meeting Abstracts(Vol. 47). | “For the New Horizons encounter with the Plutosystem, the initial satellite ephemerides (PLU043) and the initial planet and satellite masses were taken from the Brozović et al. analysis. During the New Horizons approach, the ephemerides and masses were periodically updated along with the spacecraft trajectory by the New Horizons navigation team using imaging of the planet and satellites against the stellar background.” |
| 2015 | Sekine, Y., Genda, H. and Funatsu, T., 2015, December. Can the Charon-forming giant impact generate elongated dark areas on Pluto?. In AGU Fall Meeting Abstracts. | ” Based on the satellite-to-planet mass ratio, the Pluto-Charon system is suggested to be of a giant impact origin” |
| 2015 | Showalter, M. R., and D. P. Hamilton. “Resonant interactions and chaotic rotation of Pluto/’s small moons.” Nature 522.7554 (2015): 45-49. | “Pluto and Charon comprise a ‘binary planet’—two bodies, similar in size, orbiting their common barycentre.” |
| 2015 | Stern, S.A., Porter, S. and Zangari, A., 2015. On the roles of escape erosion and the viscous relaxation of craters on Pluto. Icarus, 250, pp.287-293. | “Solar ultraviolet heating of Pluto’s upper atmosphere drives escape, causing the planet to lose 10 27 to 10 28 N 2 s −1 (eg, Zhu et al., 2014, and references therein).” |
| 2016 | Ennico, K., Parker, A., Howett, C. A. J., Olkin, C. B., Spencer, J. R., Grundy, W. M., … & Stern, S. A. (2016). Hemispherical Pluto and Charon Color Composition From New Horizons. | “Pluto Colors: We determined the blue/red color ra- tio means and standard deviations averaged over 20° longitude bins for the six data sets…The comparison of the polar and the +50° to +70° region shows that this latitudinal banding does encircle the planet.” |
| 2016 | Huang, B.C., Chou, S.W., Hong, J.M. and Yen, C.C., 2016. Global Transonic Solutions of Planetary Atmospheres in a Hydrodynamic Region—Hydrodynamic Escape Problem Due to Gravity and Heat. SIAM Journal on Mathematical Analysis, 48(6), pp.4268-4310. | “… In July 2015, the New Horizons (NH) spacecraft completed its flyby of Pluto and dis- covered flowing ice and an extended haze on the planet. Pluto exhibits a planetary geology that comprises flowing ice, exotic surface chemistry, mountain ranges, and vast haze. …” |
| 2016 | McKinnon, W.B., Moore, J.M., Spencer, J.R., Grundy, W.M., Gladstone, G.R., Nimmo, F., Schenk, P.M., Howard, A.D., Stern, S.A., Weaver, H.A. and Young, L.A., 2016, March. The Pluto-Charon system revealed: geophysics, activity, and origins. In Lunar and Planetary Science Conference (Vol. 47, p. 1995). | “New Horizons has revealed the character and evolution of a small, icy binary planet, one born in a giant impact much closer to the Sun over 4 billion years ago.” |
| 2016 | Nimmo, F., Hamilton, D.P., McKinnon, W.B., Schenk, P.M., Binzel, R.P., Bierson, C.J., Beyer, R.A., Moore, J.M., Stern, S.A., Weaver, H.A. and Olkin, C.B., 2016. Reorientation of Sputnik Planitia implies a subsurface ocean on Pluto. Nature. | “Here f is defined as f = 3m/(M + m), where m and M are the masses of the tide-raising body (Charon) and Pluto, respectively, such that for a synchronous satellite orbiting a massive planet f = 3 (yielding equation (39) of ref. 27) while for a purely rotationally distorted body f = 0.” |
| 2017 | Binzel, R.P., Earle, A.M., Buie, M.W., Young, L.A., Stern, S.A., Olkin, C.B., Ennico, K., Moore, J.M., Grundy, W., Weaver, H.A. and Lisse, C.M., 2017. Climate zones on Pluto and Charon. Icarus, 287, pp.30-36. | “Thus a consequence of Pluto’s high obliquity is that most of the planet is both tropical and arctic during the course of the 2.8 million year obliquity cycle.” |
| 2017 | Earle, A.M., Binzel, R.P., Young, L.A., Stern, S.A., Ennico, K., Grundy, W., Olkin, C.B. and Weaver, H.A., 2017. Long-term surface temperature modeling of Pluto. Icarus, 287, pp.37-46. | “This offers insight as to why the equatorial band of Pluto displays the planet’s greatest albedo contrasts.” |
| 2017 | Stern, S.A., Binzel, R.P., Earle, A.M., Singer, K.N., Young, L.A., Weaver, H.A., Olkin, C.B., Ennico, K., Moore, J.M., McKinnon, W.B. and Spencer, J.R., 2017. Past epochs of significantly higher pressure atmospheres on Pluto. Icarus, 287, pp.47-53. | “described how Pluto’s high obliquity currently causes the planet’s poles to receive moresolar insolation than does the equator over the course of an orbit.” |
Examples for Titan
| 2017 | M. J. Way, Igor Aleinov, David. S. Amundsen, Mark Chandler, Thomas Clune, Anthony D. Del Genio, Yuka Fujii, Maxwell Kelley, Nancy Y. Kiang, Linda Sohl, Kostas Tsigaridis, “Resolving Orbital and Climate Keys of Earth and Extraterrestrial Environments with Dynamics 1.0: A General Circulation Model for Simulating the Climates of Rocky Planets” Subm to Astrophys J Suppl Series (in arxiv) 2017. | “In simulating other planets, including early Earth, certain assumptions that are built into ModelE2 can become invalid, so updated or new parameterizations need to be developed for ROCKE-3D. This is especially the case for reduced atmospheres like those of Archean Earth, Titanand probably Pluto.” |
| 2017 | Zahnle, K.J. and Catling, D.C., 2017. The cosmic shoreline: the evidence that escape determines which planets have atmospheres, and what this may mean for Proxima Centauri b. arXiv preprint arXiv:1702.03386. | Constantly calls all round bodies including dwarf planets and moons “planets”. Example: “It may be reasonable to expect a lower threshold for impact erosion from planets with well-defined surfaces (Melosh and Vickery 1989), yet the different fates of Titan and Callisto can be nicely accounted for by the same factor of 4−5.” |
| 2016 | Amy, L. A., and R. M. Dorrell. “Equilibrium Conditions of Sediment Suspending Flows on Earth, Mars and Titan.” In AGU Fall Meeting Abstracts. 2016. | “to have occurred on other planets (e.g., water on Mars and methane-ethane on Titan)” “critical slopes for equilibrium flow are similar for planets. Compared to Earth, equilibrium slopes on Mars should be slightly lower whilst those on Titan will be higher or lower for organic and ice particle systems, respectively. Particle size distribution has a similar, order of magnitude effect, on equilibrium slope on each planet.“ |
| 2016 | Stevenson, David S. “Ice Dwarves: Titan, Triton and Pluto.” In The Exo-Weather Report, pp. 329-362. Springer International Publishing, 2016. | Generally careful to call Titan a moon, but it does not avoid saying the following: “Titan has an atmosphere layered much like that of Earth …. The lowest 30 km contains most of the planet’s true clouds.” and also “Titan’s low mass and its extended atmosphere should, therefore, make it vulnerable to escape, if we apply the same rules as we did to the other planets. As with the other planets, there are two main routes for escape of gases: thermal (or Jean’s escape) and several non-thermal mechanisms.” and in the following “planet” is used for several bodies including Ganymede and Titan: “All of these effects would have meant Ganymederemained largely airless while less massive Titan was able to maintain a rich, hazy firmament. There is one more factor worth considering: magnetic fields. Thinking back to Venus there is a perception that a planet must have a magnetic field if it is to retain an atmosphere against its star’s stellar wind….Ganymede has its own, relatively strong field but this is embedded within Jupiter’s enormous magnetized blanket. Titan is also within the field of Saturn, but it lies further out and Saturn’s field is around 25–30 times weaker than Jupiter’s…Under the auspices of Saturn’s field Titan, by contrast, enjoys some protection from the solar wind. Yes, there is some erosion of its atmosphere from charged particles, but this effect is far less than experienced by Jupiter’s satellites. Thus, a magnetic field may not be the protective, nourishing blanket it is always assumed to be. Venus does just fine without one, while Ganymede may have suffered because of one. Mars didn’t lose its atmosphere so much for the lack of one, but for its proximity to the Sun and its low mass. Does Titan retain an atmosphere simply because it is further from the Sun than Ganymede? In part yes.” Also, Pluto is called a dwarf planet a few times, but there is also this: “Here, the combination of greater insolation from the tilt and Pluto’s closer position to the Sun ensure the planet can begin to warm up and, at least partially, thaw out.” In comparing three bodies it calls them “worlds” in most cases, but once it calls them “dwarf planets” even though two are satellites, showing that the root noun “planet” is not a dynamical category: “Pluto, Triton and Titan form an intriguing triad of dwarf planets. While we think of Titan (quite rightly) as Saturn’s greatest moon, it has rather a lot in common with further out Triton and Pluto.” Also, Titan’s atmosphere is described as having a “planetary Hadley cell”. Not global or other. |
| 2016 | Liu, Zac Yung-Chun, Jani Radebaugh, Ron A. Harris, Eric H. Christiansen, and Summer Rupper. “Role of fluids in the tectonic evolution of Titan.” Icarus 270 (2016): 2-13. | “For example, the average slope of fold and thrust belts on terrestrial planets is commonly <15 (e.g., Yakima fold-andthrust belts in Washington, USA (Reidel, 1984) and lobate scarps on the Moon (Banks et al., 2012)).” |
| 2013 | Pascale, S., Ragone, F., Lucarini, V., Wang, Y. and Boschi, R., 2013. Nonequilibrium thermodynamics of circulation regimes in optically thin, dry atmospheres. Planetary and Space Science, 84, pp.48-65. | “… a way to estimate the meridional heat transport of other planets, such as Mars and Titan (Lorenz et al., 2001; Jupp and Cox, 2010) and potentially to exoplanets too,” |
| 2012 | Drummond, Sarah Alice. “Structural control of fluvial network morphology on Titan.” (2012). | “… by Titan’s low crater density (Lorenz et al. 2007, Wall et al. 2009, Wood et al. 2010, Neish and Lorenz 2012). For the purposes of this work external processes are defined as those for which the energy for surface modification is supplied externally to the planet’s surface.“ |
| 2010 | Lopes, R. M. C., et al. “Distribution and interplay of geologic processes on Titan from Cassini radar data.” Icarus205.2 (2010): 540-558. | “Planetary surfaces are shaped by the interplay of endogenic (volcanism, tectonism) and exogenic (impact cratering, erosion and surficial) processes. Understanding the distribution and inter- play of endogenic and exogenic processes on a planet is important for constraining models of the interior, surface–atmosphere inter- actions and climate evolution. Titan’s atmosphere is the second densest in the Solar System and present day surface–atmosphere interactions make aeolian, fluvial, pluvial, and lacustrine processes important on a scale previously seen only on Earth. and “All the major planetary geologic processes – volcanism, tecto- nism, impact cratering and erosion – have played a role in shaping Titan’s complex surface.” |
| 2010 | Vincendon, Mathieu, and Yves Langevin. “A spherical Monte-Carlo model of aerosols: Validation and first applications to Mars and Titan.” Icarus207.2 (2010): 923-931. | “This approach is relevant when the solar zenith angle is small enough to neglect the curvature of the planet (typically less than 80° for Mars and 65° for Titan, which has a larger relative scale height).” |
| 2009 | Sotin, Christophe, et al. “Titan’s interior structure.” Titan from Cassini-Huygens. Springer Netherlands, 2009. 61-73. | “This paper also describes observations and interpretations which seem difficult to reconcile with our present understanding of Titan’s interior structure and evolution such as the shape of the planet or the obliquity.” |
| 2009 | Yair, Yoav, et al. “A study of the possibility of sprites in the atmospheres of other planets.” Journal of Geophysical Research: Planets 114.E9 (2009). | “Since lightning has been found in other planetary atmospheres, it seems reasonable to assume that some form of TLEs may also occur on those planets. Detailed calculations of the conventional breakdown parameters for various planetary atmospheres have been presented lately by Roussel-Dupré et al.[2008], for a range of external electric fields. Here we present initial calculations of the necessary lightning induced charge moment changes and possible atmospheric heights for the occurrence of sprites on Venus, Mars, Titan, and the gas giant Jupiter…We calculated the values of Ek over a wide range of pressures and temperatures in each planet’s atmosphere…In order to compute the expected field above thunderclouds in other planets, we place a charge equivalent to the uppermost charge center expected in each cloud type…to account for the uncertainties in both charge locations and lightning discharge types in Venus, Titan and the giant planets… taken from the Planetary Atmospheres Node of the Planetary Data System (PDS) (http://atmos.nmsu.edu/) for Venus, Mars and Titan…” |
| 2008 | Cottin, Hervé, et al. “Heterogeneous solid/gas chemistry of organic compounds related to comets, meteorites, Titan, and Mars: laboratory and in lower Earth orbit experiments.” Advances in Space Research 42.12 (2008): 2019-2035. | “However, this planet offers an unique opportunity to study endogenous syntheses of exobiological interest since it has been shown that the hydrolysis of laboratory analogues of Titan’s organic haze (Tholins) release amino acids (Khare et al., 1986).“ |
| 2008 | Liu, Xinhua, Jianping Li, and Athena Coustenis. “A transposable planetary general circulation model (PGCM) and its preliminary application to Titan.” Planetary and Space Science 56.12 (2008): 1618-1629. | “… Firstly, since different planets have specific environments, changes were made to the model to adjust to these environments (eg, Mars, Titan and Venus): radius of the planet, acceleration of gravity, solar constant, components of the atmosphere, orbital elements…” |
| 2007 | Mitri, Giuseppe, et al. “Hydrocarbon lakes on Titan.” Icarus 186.2 (2007): 385-394. | “Cassini-Huygens observations have shown a somewhat dry planet.” |
| 2007 | Snowden, D., et al. “Three‐dimensional multifluid simulation of the plasma interaction at Titan.” Journal of Geophysical Research: Space Physics 112.A12 (2007). | “When the plasma flows near Titan the plasma that encounters Titan’sionosphere is slowed and the frozen-in field lines are forced to drape around the planet.” |
| 2006 | Barth, Erika L., and Owen B. Toon. “Methane, ethane, and mixed clouds in Titan’s atmosphere: Properties derived from microphysical modeling.” Icarus 182.1 (2006): 230-250. | “Titan’s most visible feature is the optically thick haze layer enveloping the planet about 200 km above the surface.” |
| 2005 | Kostiuk, T., et al. “Titan’s stratospheric zonal wind, temperature, and ethane abundance a year prior to Huygens insertion.” Geophysical research letters32.22 (2005). | “The FOV shown in Figure 1 covers an extended portion of Titan with varying viewing angle and line-of-sight velocity projection…For the 0.5″ visible seeing profile, the effective beam width at 12 μm on the planet was ~ 0.4″ FWHM.” |
| 2005 | Moreno, R., A. Marten, and T. Hidayat. “Interferometric measurements of zonal winds on Titan.” Astronomy & Astrophysics 437.1 (2005): 319-328. | “Since the planet rotation is slow (11.7 m/s), Titan’s atmosphere is observed in superrotation, similar to that of Venus (Schubert 1983), the only other known case.” |
| 2004 | Elachi, Ch, et al. “Radar: the Cassini Titan radar mapper.” Space Science Reviews 115.1-4 (2004): 71-110. | “The post-Voyager value of Titan’s density, 1.88 g cm−3 (Tyler et al., 1981; Lindal et al., 1983), allows for a silicate abundance comparable to or less than that of ices and organics together. The suspended aerosol particles represent one end state of the photolysis of methane, which also results in the escape of hydrogen from the planet.” |
| 2004 | Simakov, M. B. “Possible biogeochemical cycles on Titan.” Origins. Springer Netherlands, 2004. 645-665 | “The time of existence of the Titan’s juvenile ocean was enough for arising of the first protoliving objects. As the planet developed through time several energetic processes (irradiation, lightnings,meteoritic and comet impacts) could produce different forms of fixed nitrogen…” |
| 2003 | Luna, H., et al. “Dissociation of N2 in capture and ionization collisions with fast H+ and N+ ions and modeling of positive ion formation in the Titan atmosphere.” Journal of Geophysical Research: Planets108.E4 (2003). | “Titan’s atmosphere is also unusually large due to its much smaller gravity. That is, the exobasealtitude, the altitude above which escape occurs and below which the atmosphere is collisional, is about 60% of the planet’s radius (~1500 km)” |
| 2003 | Westhelle, Carlos, and James Masciarelli. “Assessment of aerocapture flight at Titan using a drag-only device.” AIAA Atmospheric Flight Mechanics Conference and Exhibit. 2003. | “For the Titan aerocapture trajectory simulations, the planet and gravity model used are a spherical body of radius 2575 km with an inverse square gravity field with a gravitational parameter of 9.1420 × 103 km3/s2.“ |
| 2002 | Hall, Jeffery L., et al. “Titan airship explorer.” Aerospace Conference Proceedings, 2002. IEEE. Vol. 1. IEEE, 2002 | “On the other hand, the dense atmosphereand low temperature contrasts makes Titan almost an ideal planet for aerial vehicles.” |
| 2001 | Kerzhanovich, V., et al. “Titan airship surveyor.” Forum on Innovative Approaches to Outer Planetary Exploration 2001-2020. Vol. 1. 2001. | “…makes Titan the almost ideal planet for studies with lighter-than-air aerial platforms…” |
| 2000 | Brecht, Stephen H., Janet G. Luhmann, and David J. Larson. “Simulation of the Saturnian magnetospheric interaction with Titan.” Journal of Geophysical Research: Space Physics 105.A6 (2000): 13119-13130. | “180 ø is on the midnight side of the planet, and 270 ø is on the side of Titan where the Econv is pointing into the surface of the planet. … |
| 2000 | Banaszkiewicz, M., et al. “A Coupled Model of Titan’s Atmosphere and Ionosphere” Icarus 147, 386-404 (2000). | “In the case of Titan, the field lines pile up near the subram point on the leading side of Titan and then turn gently toward the flanks of the planet.” |
| 1998 | Forget, F. “Habitable zone around other stars.” Earth, Moon, and Planets 81.1 (1998): 59-72. | “As for Venus and Titan the atmosphere rotates much faster than the solid planet at most level …” |
| 1996 | Del Genio, Anthony D., and Wei Zhou. “Simulations of superrotation on slowly rotating planets: Sensitivity to rotation and initial condition.” Icarus120.2 (1996): 332-343. | “…the eddy momentum effect of the prograde rotation of the solid planet will determine the sense of atmospheric rotation on Titan.” |
| 1996 | Hourdin, Frederic, et al. “Numerical modelling of the circulation of superrotating atmospheres: Venus and Titan.” Environment Modeling for Space-Based Applications. Vol. 392. 1996. | “… performed with the Titan atmospheric GCM also produced a strong stratospheric superrotation with prograde winds of the order of 100 rn/s at the equator and an upper stratosphere rotating about 10 times faster than the solid planet (the rotation period of Titan, assumed to be …” |
| 1995 | Hourdin, Frédéric, et al. “Numerical simulation of the general circulation of the atmosphere of Titan.” Icarus117.2 (1995): 358-374. | “After 1.5 Titan years, the upper stratosphere rotates about 9 times faster than the solid planet and this superrotation still increases at the end of the simulation.” |
| 1995 | Lunine, J. I., and C. P. McKay. “Surface-atmosphere interactions on Titan compared with those on the pre-biotic Earth.” Advances in Space Research 15.3 (1995): 303-311. | “Therefore, study of Titan through the Cassini/Huygens mission, planned for launch in1997, primarily affords the opportunity to understand planet-wide surface-atmosphere interactions in the presence of fluids but in the absence of life.” |
| 1993 | Del Genio, Anthony D., Wei Zhou, and Timothy P. Eichler. “Equatorial superrotation in a slowly rotating GCM: Implications for Titan and Venus.” Icarus 101.1 (1993): 1-17. | “In principle, the simplest test of superrotation theories would be a direct simulation of the Venus and Titan atmospheres, with accurate specifications of atmospheric mass and composition,radiative heating, and planetary radius and surface properties for each planet.” |
| 1992 | Hourdin, F., et al. “Numerical simulation of the circulation of the atmosphere of Titan.” Symposium on Titan. Vol. 338. 1992. | “A three dimensional General Circulation Model (GCM) of Titan‘s atmosphere is described…It appears that for a slowly rotating planet which strongly absorbs solar radiation, circulation is dominated by global equator to pole Hadley circulation and strong superrotation.” |
| 1992 | Raulin, F. “Titan: a prebiotic planet?.” Frontiers of Life. 1992. | “Titan: a prebiotic planet?” |
| 1988 | Toon, Owen B., et al. “Methane rain on Titan.” Icarus 75.2 (1988): 255-284. | “If optically thick methane clouds were present then one might expect to see their effects on the planet’s radiation balance at visible wavelengths.” |
| 1984 | Thompson, W. Reid, and Carl Sagan. “Titan: Far-infrared and microwave remote sensing of methane clouds and organic haze.” Icarus 60.2 (1984): 236-259. | “…ray paths through the atmosphere, with atmospheric sphericity (and in fact emission from beyond the solid disk of the planet)…” |
| 1975 | Bunten, Donald M. “The outer planets.” Scientific American 233, no. 3 (1975): 130-141. | “Although Titan is a satellite of Saturn, it is appropriate to discuss it here as a planet. It is larger than Mercury and almost as large as Mars. It has an atmosphere that is deeper than that of Mars…” (etc., describing planetary qualities) |
| 1966 | Kalinyak, A. A. “Data on the Spectra of the Galilean Satellites of Jupiter.” Soviet Astronomy 9 (1966): 824. | “The discover of kuiper of an atmosphere on Titan provided definitive proof of the possible existence of gaseous envelopes in an equilibrium state on minor planets having masses of the order of the lunar mass. The mass ratio of Titan and the moon is 1.9. (new para.) The physical conditions prevailing on the surface of the planet impose certain requirements ont he chemical composition of their atmospheres…” |
Examples for Europa
| 2019 | Shi, Erbin, Alian Wang, and Zongcheng Ling. “MIR, VNIR, NIR, and Raman spectra of magnesium chlorides with six hydration degrees: Implication for Mars and Europa.” Journal of Raman Spectroscopy 51, no. 9 (2020): 1589-1602. | “The observations by the Galileo and Cassini‐Huygens missions at Europa have found deep oceans at this planet with evidence for the presence of salts.” |
| 2015 | Bayer, Todd, Brian Cooke, I. Gontijo, and Karen Kirby. “Europa Clipper Mission: the habitability of an icy moon.” In 2015 IEEE Aerospace Conference, pp. 1-12. IEEE, 2015. | Europa is unique among the large icy satellites because its liquid water ocean is believed to be in direct contact with its rocky mantle, where conditions could be similar to those on Earths biologically rich sea floor. Hydrothermal zones on the sea floor are known to be rich with life, providing energy from deep in the planet’s core and nutrients from reactions between the seawater and the warm rocky ocean floor. |
| 2010 | Greenberg, Richard. Unmasking Europa: The search for life on jupiter’s ocean moon. Vol. 6. Springer Science & Business Media, 2010. | “But information about the surface of Europa came from images taken of an alien planet using a telescope flying through space.”, and, “But there is a danger in unduly applying terrestrial experience to a planet that may be completely different. The initial considerations of Europa were based upon comparisons with the most similar types of familiar geological features on Earth.” And “This picture has emerged as we have come to know Europa as a planet. … Unmasking Europa physical processes were actually responsible for the character of the planet.” |
| 2009 | Blanc, Michel, et al. “LAPLACE: A mission to Europa and the Jupiter System for ESA’s Cosmic Vision Programme.” Experimental Astronomy23.3 (2009): 849-892. | “… All these topics relate to whether a planet immersed in a strong radiation environment can host complex compounds able to react chemically.” |
| 2008 | Leighton, Timothy G., Daniel C. Finfer, and Paul R. White. “The problems with acoustics on a small planet.” Icarus193.2 (2008): 649-652. | “To do so would be to assume a constant acceleration due to gravity, and to ignore the curvature of Europa’s spherical geometry: vertical lines are not parallel on a small planet…Dotted curve (. . .) plots c2, the sound speed calculated ignoring planetcurvature and for a gravitational acceleration which is constant at a value of 1.31 m s-2 (the value at Europa’s surface)…On a small planet…a planetresembling Europa…” |
| 2005 | Lipps, Jere H., and Sarah Rieboldt. “Habitats and taphonomy of Europa.” Icarus177.2 (2005): 515-527. | “Clearly, an adequate assessment of life on another planet requires multiple instruments and techniques.” |
| 2005 | Mitri, Giuseppe, and Adam P. Showman. “Convective–conductive transitions and sensitivity of a convecting ice shell to perturbations in heat flux and tidal-heating rate: Implications for Europa.” Icarus177.2 (2005): 447-460. | “… Structures and temperature profiles for two possible configurations of the ice shell of Europa. The heat generated in the interior of the planet might be shed by simple conduction through a relatively thin ice shell…” |
| 2003 | Marion, Giles M., et al. “The search for life on Europa: limiting environmental factors, potential habitats, and Earth analogues.” Astrobiology 3.4 (2003): 785-811. | “Two aspects of time have a bearing on the possibility of life on Europa: (1) How much time is required for life to develop on a planet? (2) How long can life survive in the dormant stage in iso- lation from conditions normally considered vital for life such as cycling of liquid water, energy, and nutrients?” |
| 2002 | Sotin, Christophe, James W. Head, and Gabriel Tobie. “Europa: Tidal heating of upwelling thermal plumes and the origin of lenticulae and chaos melting.” Geophysical Research Letters 29.8 (2002). | “the viscous response of the planet is considered as a first order perturbation of the elastic response to the tidal potential” |
| 2002 | Sotin, Christophe, James W. Head, and Gabriel Tobie. “Europa: Tidal heating of upwelling thermal plumes and the origin of lenticulae and chaos melting.” Geophysical Research Letters 29.8 (2002). | “the viscous response of the planet is considered as a first order perturbation of the elastic response to the tidal potential” |
| 2000 | Kivelson, Margaret G., et al. “Galileo magnetometer measurements: A stronger case for a subsurface ocean at Europa.” Science289.5483 (2000): 1340-1343. | “… The Galileo magnetometer measured changes in the magnetic field predicted if a current-carryingouter shell, such as a planet-scale liquid ocean, is present beneath the icy surface. The evidence that Europa’sfield varies temporally strengthens the argument that a liquid ocean …” |
| 2000 | Mitri, Giuseppe, and Adam P. Showman. “Convective–conductive transitions and sensitivity of a convecting ice shell to perturbations in heat flux and tidal-heating rate: Implications for Europa.” Icarus177.2 (2005): 447-460. | “… Structures and temperature profiles for two possible configurations of the ice shell of Europa. The heat generated in the interior of the planet might be shed by simple conduction through a relatively thin ice shell…” |
| 2000 | Phillips, Cynthia B., et al. “The search for current geologic activity on Europa.” Journal of geophysical research105.E9 (2000): 22579-22598. | “Figure 2b, with the bright limb at 7% of its fullbrightness, shifted off the planet by 16 pixels.” |
| 1989 | Ojakangas, Gregory W., and David J. Stevenson. “Polar wander of an ice shell on Europa.” Icarus81.2 (1989): 242-270. | “The problem is that of a planetary elastic lithosphere that is topographically loaded from below.” And “We describe one such scenario: that of a planet with an elastic lithosphere which is topographically loaded from below. We describe how this scenario applies to the question of polar wander of Europa,…” |
| 1989 | Schenk, Paul M., and William B. McKinnon. “Fault offsets and lateral crustal movement on Europa: Evidence for a mobile ice shell.” Icarus79.1 (1989): 75-100. | “… across the wedge-shaped band rift zone is limited to a relatively small area, and may have been taken up planet-wide by … “ |
| 1981 | Finnerty, A. A., et al. “Is Europa surface cracking due to thermal evolution.” Nature 289 (1981): 24-27. | “It is proposed that some of the surface features of Europa may be due to processes occurring within a planet in which hydrated silicates are stable.” |
Examples for the Moon
| 2013 | Gudkova, T. V., and S. N. Raevskii. “Spectrum of the free oscillations of the Moon.” Solar System Research 47.1 (2013): 11-19. | “The model of the planet is considered as a sphere of equivalent volume…The amplitudes of these functions are normalized to unity at the surface of the Moon…Since the torsional oscillations are only associated with the solid planet’s regions…The free oscillations have an important property: they move toward the surface of the planet as the oscillation number increases. Therefore, different frequency intervals of the free oscillations are determined by the properties of different regions of the Moon’s interior.” |
| 2007 | Sherwood, Brent. “What Will We Actually Do On the Moon?.” AIP Conference Proceedings. Ed. Mohamed S. El-Genk. Vol. 880. No. 1. AIP, 2007. | “… A convenient taxonomy divides them into science of the Moon (history and evolution of the Moon as a planet), science on the Moon (including science underlying the activities discussed in the previous section), and science from the Moon (such as astronomy). …” |
| 2007 | Wieczorek, Mark A. “Gravity and topography of the terrestrial planets.” Treatise on Geophysics.–2007.–10 5 (2007): 165-206. | “Gravity and Topography of the Terrestrial Planets…Earth, Venus, Mars, the Moon” |
| 1991 | , “Lunar Minerals” in Lunar Sourcebook, Heiken, Grant H., David T. Vaniman, and Bevan M. French. (Eds), Cambridge, England, Cambridge University Press, 1991, | “The major differences between the oxide minerals in lunar and terrestrial rocks arise from fundamental differences between both the surfaces and the interiors of these two planets.” |
| 1988 | Watters, Thomas R. “Wrinkle ridge assemblages on the terrestrial planets.” Journal of Geophysical Research: Solid Earth 93.B9 (1988): 10236-10254. | “Wrinkle ridge assemblages on the terrestrial planets…Moon, Mars, and Mercury.” |
| 1981 | Murray, Bruce, Michael C. Malin, and Ronald Greeley. “Earthlike Planets: Surfaces of Mercury, Venus, Earth, Moon, Mars.” Research supported by the John Simon Guggenheim Memorial Foundation and California Institute of Technology. San Francisco, WH Freeman and Co., 1981. 402 p. 1 (1981). | “Earthlike planets: Surfaces of Mercury, Venus, earth, moon, Mars” |
| 1981 | Head, James W., and Sean C. Solomon. “Tectonic evolution of terrestrial planets.” Science 213, no. 4503 (1981): 62-76. | “Tectonic evolution of terrestrial planets.” (Includes an entire section on the Moon and extensive comparison of terrestrial planets including the Moon as “planets”) “The style and evolution of tectonics on the terrestrial planets differ substantially. The style is related to the thickness of the lithosphere and to whether the lithosphere is divided into distinct, mobile plates that can be recycled into the mantle, as on Earth, or is a single spherical shell, as on the moon, Mars, and Mercury. The evolution of a planetary lithosphere and the development of plate tectonics appear to be influenced by several factors, including planetary size, chemistry, and external and internal heat sources.” “Tectonics and thermal history are also closely related on planets that lack laterally mobile lithospheric plates (the moon, Mars, and Mercury).” “Fig. 3. Interiors of the terrestrial planets. For the moon, a 70-km-thick crust is indicated…” “an early period of modest global expansion and lithospheric extension is confined to the first 1.0 billion years of lunar history. This extensional period is followed by a more extended period of modest planetary contraction and lithospheric compression lasting until the present…” “At least since the formation of a thick global crust the moon has been a one-plate planet.” “The Mariner 9 and Viking missions to Mars revealed a planetary surface more geologically complex than that of the moon or Mercury…” “Mars, like the moon and probably Mercury, is a differentiated planet…” “The deformation of Earth’s lithosphere by volcanic loads is a direct analog to the loading of a planetary lithosphere by basalt fill in a large basin, as on the moon, or by a volcanic construct, as on Mars.” “The plate tectonic cycle has dominated the heat budget of the outer several hundred kilometers of Earth and has led to a level of volcanic activity which, when integrated through time, surpasses by a huge factor that seen on the moon, Mercury, or Mars. Earth shares with the other terrestrial planets, however, the concept of the lithosphere as an important governor of tectonic style. The vertical tectonics on Earth associated with volcanic loading, continental rifting, and subsidence of continental margins and plat- form basins has many direct analogs on the other planets.” “The influence of major changes in the interior and exterior environment of a planet are often readily visible on one-plate planets.” |
| 1980 | Phillips, Roger J., and Kurt Lambeck. “Gravity fields of the terrestrial planets: Long‐wavelength anomalies and tectonics.” Reviews of Geophysics 18.1 (1980): 27-7 | “We present a review of the long-wavelength gravity fields of the terrestrial planets, earth, moon, Mars, and Venus…” |
| 1980 | Pollack, James B., and Yuk L. Yung. “Origin and evolution of planetary atmospheres.” Annual Review of Earth and Planetary Sciences 8, no. 1 (1980): 425-487. | This work generally separates planets from satellites. However: “Thermal evolution of the interiors of the Moon (a), Mercury (b), Mars (c), and Venus (d) as a function of time from the completion of planetary formation (0 years). The curves in these figures are isutherms, with their associated numbers being temperatures in dc. In all cases, the model planets were assumed to have a homogeneous composition at the initial epoch” Whenever it speaks of the general case (for all planets and satellites), it says “planet”. Here’s an example, where it shortly after includes the Moon: “Assuming solar wind sweeping operates at maximum efficiency, one may write this escape flux, Fs.w., as (Hunten & Donahue 1976) (Equation here), (6) where ¢, H, and r are the flux of solar wind protons, atmospheric scale height at the level of the solar wind, and distance from the center of the planet to the interface with the solar wind near the limb, respectively. Solar wind sweeping represents an important loss process for C and N from Mars (McElroy 1 972), for H from Venus (Kumar et al 1 978), and for all the constituents of the lunar atmosphere (Kumar 1976). |
| 1979 | Schubert, Gerald. “Subsolidus convection in the mantles of terrestrial planets.” Annual review of earth and planetary sciences 7.1 (1979): 289-342 | “Each of the terrestrial planets, Mercury, Venus, Earth, Moon and Mars…” |
| 1979 | Solomon, Sean C. “Formation, history and energetics of cores in the terrestrial planets.” Physics of the Earth and Planetary Interiors 19.2 (1979): 168-182. | “The cores of the terrestrial planets Earth, Moon, Mercury, Venus and Mars differ…” |
| 1978 | Warner, J. L., and D. A. Morrison. “Planetary Tectonics i: the Role of Water.” Lunar and Planetary Science Conference. Vol. 9. 1978. | “Essentially all thermal models for terrestrial planetswhich have been calculated since the first samples were returned from the Moon contain a stage early in each planet’s history where at least the outermost few hundred km were molten…” |
| 1977 | Head, James W., Charles A. Wood, and Thomas A. Mutch. “Geologic Evolution of the Terrestrial Planets: Observation and exploration have yielded fundamental knowledge of planetary evolution and have given rise to an exciting new view of Earth as a planet.” American Scientist 65.1 (1977): 21-29. | “The style and evolution of tectonics on theterrestrial planets differ substantially. The style is related to the thickness of the lithosphere and to whether the lithosphere is divided into distinct, mobile plates that can be recycled into the mantle, as on Earth, or is a single spherical shell, as on the moon, Mars,and Mercury.” and “Tectonics and thermal history are also closely related on planets that lack laterally mobile lithospheric plates (the moon, Mars, and Mercury)” |
| 1966 | Fielder, G. “Convection in the Moon: a boundary condition.” Geophysical Journal International10.4 (1966): 437-443. | “Convection in the Moon: A Boundary Condition…Convective motion in a solid planet may be expected to produce surface configurations that are a consequence of, and to this extent characterize, the motion beneath the surface…Several authors have observed a pattern of lineaments, or ‘grid system’ on the Moon…” |
Ceres
| 2020 | https://www.nasa.gov/mediacast/gravity-assist-the-bright-spot-of-the-asteroid-belt-with-britney-schmidt | Britney Schmidt: It’s the innermost icy world, and a miniature version of maybe what some of the other planets looked like early on. It’s one of the only planetsthat’s really made of this kind of frozen ground on the, on the outside. So I kind of like to call it a permafrost planet, if you will. So if you think about the Arctic on the Earth, where the ground is frozen, year round, it’s the same thing on Ceres. It’s kind of this frozen mud up on top. So that’s kind of special. And it’s really a weird object in that way. It has something in common with Mars has something in common with the Earth and with places like Europa and Enceladus in the outer solar syste. But we call it a dwarf planet, it basically means that it is round, as you say, and so it has self-gravity, it’s done some really interesting things that planets do. So when you picture an asteroid being like kind of a twisted hunk of metal or rock, then you’re really missing the picture with Ceres, which is a big sphere, made of this kind of ice-rich, rocky material |
| 2015 | McCord, T., and Dawn Team. “Dawn: A journey in space and time.” EGS-AGU-EUG Joint Assembly. 2003. | “Dawn provides the missing context for both primitive and evolved meteoritic data, thus playing a central role in understanding terrestrial planet formation and the evolution of the asteroid belt.” |
| 2015 | Russell, Christopher T., et al. “First Results of the Exploration of Ceres by Dawn.” IAU General Assembly 22 (2015): 21738. | “The first comprehensive survey of the planet is scheduled to commence in late April 2015,…” |
| 2015 | Villarreal, M. N., et al. “Evidence for a Bow Shock at Ceres?.” AGU Fall Meeting Abstracts. 2015. | “The spikes were consecutively located closer to the planet as the spacecraft approached the subsolar point. The dramatic increase in electron counts could be explained by the acceleration of the electrons at a Ceresbow shock.” |
| 2015 | Rambaux, N., F. Chambat, and J. C. Castillo. “Third-Order Development of Shape, Gravity, and Moment of Inertia of Ceres.” AGU Fall Meeting Abstracts. 2015. | “interpreting shape and gravity data in terms of interior structure and infer deviations from hydrostaticity that can bring information on the thermal and chemical history of the planet.” |
| 2014 | McCord, T. “Ceres: Dawn visits a warm wet planet.” European Planetary Science Congress 2014, EPSC Abstracts, Vol. 9, id. EPSC2014-96. Vol. 9. 2014. | “Ceres likely contains considerable water, has differentiated, possesses a silicate core and water mantle, and has experienced major dimensional, thermal and chemical changes over its history, making it more a planet than an asteroid.” |
| 2013 | McCord, T. “Ceres: Evolution and What Dawn Might Find.” European Planetary Science Congress 2013, held 8-13 September in London, UK. Online at: http://meetings. copernicus. org/epsc2013, id. EPSC2013-129. Vol. 8. 2013. | “Ceres likely contains considerable water, has differentiated, and has experienced majordimensional and chemical changes over its history, making it more a planetthan asteroid” |
| 2003 | McCord, T. B., and C. Sotin. “The small planet Ceres: Models of evolution and predictions of current state.” Bulletin of the American Astronomical Society. Vol. 35. 2003. | “The Small Planet Ceres: Models of Evolution and Predictions of Current State” |
| 2003 | Mccord, T. B., and C. Sotin. “The small planet Ceres: Predictions of current state.” EGS-AGU-EUG Joint Assembly. 2003. | “Ceres orbits the sun and is large enough (1000 km diameter) to have experienced many of the processes normally associated with planetary evolution. Therefore, it should be called a planet even though it orbits in the middle of the asteroid belt.” |
| 2003 | McCord, T., and Dawn Team. “Dawn: A journey in space and time.” EGS-AGU-EUG Joint Assembly. 2003. | “Dawn provides the missing context for both primitive and evolved meteoritic data, thus playing a central role in understanding terrestrial planet formation and the evolution of the asteroid belt.” |
| 1996 | Hantzsche, E. “Planet Ceres.” Die Sterne 72 (1996): 125-133. | “Planet Ceres” |
| 1989 | Rambaux, N., F. Chambat, and J. C. Castillo. “Third-Order Development of Shape, Gravity, and Moment of Inertia of Ceres.” AGU Fall Meeting Abstracts. 2015. | “interpreting shape and gravity data in terms of interior structure and infer deviations from hydrostaticity that can bring information on the thermal and chemical history of the planet.” |
| 1983 | Johnson, Paul E., et al. “10 μm polarimetry of ceres.” Icarus56.3 (1983): 381-392. | “POLARIMETRY OF CERES For a spherical planet the net polarization will increase asthe sphere is viewed at angles such that the subsolar point is seen closer to the limb,…” |
| 1981 | Taylor, G. E. “Occultations of stars by the four largest minor planets, 1981-1989.” The Astronomical Journal 86 (1981): 903-905. | “the orbital latitude of the planet.” [Ceres] |
| 1980 | Branham, Richard L. “Equinox and equator determinations from hypothetical minor planet observations.” Celestial Mechanics and Dynamical Astronomy 22.1 (1980): 81-87 | “…shows the number of minor planets in the solution and the number in parentheses is the numerical designation of the planet,…” |
| 1977 | Hodgson, Richard G. “Implications of Recently Published Diameters for 1 Ceres, 2 Pallas and 4 Vesta.” Minor Planet Bulletin 5 (1977): 8-11. | “The writer would like to propose a different model for Ceres which would keep some or all of the interpretations of surface materials as live possibilities, and yet explain the low density of the planet.” |
| 1975 | Boiko, V. N. “Improvement of the fundamental-catalog system for minor-planet observations.” Soviet Astronomy 19 (1975): 261-266. | “We have carried out several solutions for the planetCeres, making the following changes in its orbital elements:…” |
| 1974 | Hodgson, Richard G. “The Densities of Pallas and Vesta and their Implications.” Minor Planet Bulletin 2 (1974): 17-20. | “This problem has previously been discussed in relation to the planet Ceres” |
Examples for Triton
| 2017 | Strobel, D.F., and X. Zhu 2017. Comparative planetary nitrogen atmospheres: Density and thermal structures of Pluto and Triton. Icarus 291, 55-64. | Refers to Triton and Pluto as “these icy planetary bodies”. |
| 2016 | Hall III, James A. “Neptune.” In: Moons of the Solar System. Springer International Publishing, 2016. 171-184. | “Triton destroyed and further doomed other moons, and Neptune has in turn doomed Triton. The planet is expected to pass by the Roche limit or crash into Neptune’s atmosphere in about 3.6 billion years…” |
| 2015 | Trafton, L.A. 2015. On the state of methane and nitrogen ice on Pluto and Triton: Implications of the binary phase diagram. Icarus 246, 197-205. | Refers to Triton and Pluto as “these two dwarf planets”. |
| 2013 | Zalucha, A.M., and T.I. Michaels 2013. A 3D general circulation model for Pluto and Triton with fixed volatile abundance and simplified surface forcing. Icarus 223, 819-831. | Regularly uses the term “planetary atmospheres” in speaking about both Pluto and Triton. |
| 2012 | Gaeman, J., S. et al. 2012. Sustainability of a subsurface ocean within Triton’s interior. Icarus 220, 339-347. | “Ross and Schubert (1990) argue that during the circularization of Triton, enough heat was generated to melt the entire planet.” |
| 2012 | Tegler, S.C., et al. 2012. Ice mineralogy across and into the surfaces of Pluto, Triton, and Eris. Astrophys. J. 751, 76.1-10. | Regularly uses the term “dwarf planet” for Pluto, Triton, and Eris. |
| 2011 | Gaeman, J. S. (2011). Crystallization of a Subsurface Ocean on Triton(Doctoral dissertation). | “One hypothesis suggests that Triton was captured via binary-planet exchange, whereby Triton and a second body of similar size formed a binary system with the Sun” |
| 2009 | Rosaev, A. “Numeric modeling binary asteroid gravitational encounter with Jupiter.” European Planetary Science Congress 2009. Vol. 1. 2009. | “Neptune’s capture of its moon Triton in a binary-planet gravitational encounter.” |
| 2005 | Prockter, L.M., et al. 2005. A shear heating origin for ridges on Triton. Geophys. Res. Lett. 32, L14202.1-4. | “…both moons show linear ridges with similar morphologies that are not observed on any other planetary bodies” (referring to Triton and Europa). |
| 2000 | Elliot, J.L., et al. 2000. The thermal structure of Triton’s middle atmosphere. Icarus 143, 425-428. | Regularly uses the word “planetary” to refer to radius and boundary layer in a paper about Triton. |
| 1997 | Olkin, C.B., et al. 1997. The thermal structure of Triton’s atmosphere: Results from the 1993 and 1995 occultations. Icarus 129, 178-201. | Repeatedly uses the word “planet” when describing the modeling approach used for Triton’s atmosphere. |
| 1993 | Krasnopolsky, V.A., et al. 1993. Temperature, N2, and N density profiles of Triton’s atmosphere: Observations and model. J. Geophys. Res. 98, 3065-3078. | “The total escape flux from a planet is … in the case of the atomic nitrogen escape from Triton when …” |
| 1992 | Bazilevskii, A.T., et al. 1992. Geology of Triton and some comparative-planetological implications. Adv. Space Res. 12, 123-132. | “…subsequent cooling of the planet interiors.” |
| 1992 | Lee, P., et al. 1992. Anomalous-scattering region on Triton. Icarus 99, 82-97. | Appendix: “…disk resolved photometric behavior of a planetary surface.” |
| 1992 | Spencer, J.R., and J.M. Moore 1992. The influence of thermal inertia on temperatures and frost stability on Triton. Icarus 99, 261-272. | “By analogy with other solid planetary surfaces, any nonporous substrate on Triton is …” |
| 1992 | Stansberry, J.A., et al. 1992. Triton’s surface-atmosphere energy balance. Icarus 99, 242-260. | “The scope of this study is confined to the planetary boundary layer of Triton where…” |
| 1991 | Grundy, W.M., and U. Fink 1991. A new spectrum of Triton near the time of the Voyager encounter. Icarus 93, 379-385. | “A successful model must account for multiple scattering of photons, shadowing, and other complications expected to occur on real planetary surfaces.” |
| 1991 | Stern, S.A., et al. 1991. Rotationally resolved midultraviolet studies of Triton and the Pluto/Charon system I: IUE results. Icarus 92, 332-341. | “…near IAU’s performance limit for these dim, planetary targets.” (referring to both Pluto and Triton). |
| 1990 | Soderblom, L.A., et al. 1990. Triton’s geyser-like plumes: Discovery and basic characterization. Science 250, 410-415. | “These are projected onto a model of the planet’s surface, in this case a sphere…” |
| 1990 | Nelson, R.M., et al. 1990. Temperature and thermal emissivity of the surface of Neptune’s satellite Triton. Science 250, 429-431. | “..reflectance properties of candidate materials of planetary surfaces.” |
| 1990 | Ingersoll & Tryka 1990. Triton’s plumes: The dust devil hypothesis. Science 250, 435-437. | “Planetary bodies with thin atmospheres are more likely to have dust devils than those with thick atmospheres.” |
| 1990 | Ingersoll, A.P. 1990. Dynamics of Triton’s atmosphere. Nature 344, 315-317. | “…much less than Triton’s tangential speed of rotation … where Omega is the angular velocity of the solid planet.” and “…solar heating at the equator is comparable to that for the planet as a whole.” |
| 1990 | Spencer, J.R., et al. 1990. Solid methane on Triton and Pluto: 3- to 4-micron spectrophotometry. Icarus 88, 491-496. | “The model assumes a clear atmosphere overlaying a diffusely scattering uniform spherical planet.” (model is applied both to Pluto and Triton) |
| 1989 | Stansberry, J.A. 1989. Albedo patterns on Triton. Geophys. Res. Lett. 16, 961-964. | “…fresh frost layer covering approximately the northern half of the planet.” |
| 1989 | Stern, S.A. 1989. Implications of the stability and radiative time constant of Triton’s atmosphere. Geophys. Res. Lett. 16, 977-980. | “…fraction of Triton’s mass lost as a function … and a bulk planetary density of 2.0 g cm^-3.” |
Miscellaneous Additional Examples
| 2012 | Cessateur, Gaël, et al. “Photoabsorption in Ganymede’s atmosphere.” Icarus 218.1 (2012): 308-319. | “Photolysis in Ganymede’s atmosphere…case 3 is when the spacecraft looks at the surface of the planet (limb viewing).” |
| 2011 | Schlichting, Hilke E. “Runaway growth during planet formation: Explaining the size distribution of large Kuiper Belt objects.” The Astrophysical Journal728.1 (2011): 68. | See title. KBOs were made by “planet formation.” |
| 2008 | Kenyon, Scott J., and Benjamin C. Bromley. “Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 M☉ Main-Sequence Stars.” The Astrophysical Journal Supplement Series 179.2 (2008): 451. | “3. PLANET FORMATION CALCULATIONS “Icy Planet Formation in Disks around 1 M⊙ Stars “We begin with a discussion of planet formation in disks at 30–150 AU around a 1 M⊙ star. For most disks around low mass stars, the timescale for planet formation is shorter than the main sequence lifetime. Thus, the growth of planetesimals into planets and the outcome of the collisional cascade depend more on the physics of solid objects than on stellar physics. Here, we review the stages in planet growth and describe the outcome of the collisional cascade. For a suite of calculations of planet formation in disks of different masses, we derive basic relations for the growth time and the maximum planetmass as a function of initial disk mass. We also show how the dust production rate and the mass in small objects depend on initial disk mass and time.” (Note at this distance these are icy dwarf planets) |
| 1996 | Kivelson, M. G., et al. “A magnetic signature at Io: Initial report from the Galileo magnetometer.” Science273.5273 (1996): 337. | “It seems plausible that Io, like Earth and Mercury, is a magnetized solid planet.” |
| 1964 | Binder, A.B. and Cruikshank, D.P., 1964. Evidence for an atmosphere on Io. Icarus, 3(4), pp.299-305. | “Thus, if only 10% of the maximum available CH.f froze out during the eclipse over 20% of the planet, the resulting layer would be…” |