Planets Classification

Total Page：16

File Type：pdf, Size：1020Kb

Planets Classification Our solar system contains 8 primary planets and Pluto, which is a Dwarf Planet. These 8 primary planets are: Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus and Neptune. Out of these 8, the first 4 are Terrestrial planets while the other 4 are Jovian planets. Among the Jovian planets, Jupiter and Saturn are gas giants while Uranus and Neptune are ice giants. Some of these planets have satellites and moons. For example, Mars has 2 moons called Phobos and Deimos. Write an algorithm using Python that: 1. Ask the user to manually input a planet in the solar system 2. Output {name} is a Terrestrial planet if the user chose Mercury, Venus, Earth or Mars 3. Output {name} is a Jovian planet if the user chose Jupiter, Saturn, Uranus or Neptune 4. Output {name} is a Dwarf planet if the user chose Pluto 5. Output {name} is also a gas giant if the user chose either Jupiter or Saturn 6. Output {name} is also an ice giant if the user chose either Uranus or Neptune 7. If the user chose Mars, output “Mars has 2 moons, Phobos and Deimos” 8. If the user chose Jupiter, output “Jupiter has 4 satellites, 46 moons and 17 provisional moons” 9. If the user chose Saturn, output “Saturn has 7 satellites, 46 moons, 3 Trojan moon groups and 9 provisional moons” 10. If the user chose Uranus, output “Uranus has 5 satellites and 23 moons” 11. If the user chose Pluto, output “Pluto has 1 satellite and 4 moons” 12. Make sure that the name of the planet in the output section is always capitalized An example of the output where the user has input ‘jupiter’ is: Jupiter is a Jovian planet Jupiter is a gas giant Jupiter has 4 satellites, 46 moons and 17 provisional moons Note that the user has input ‘jupiter’ but the output came out as ‘Jupiter’, which follows the rule given by #12. .

Copy Link

Recommended publications

Mars Mars Is the Fourth Terrestrial Planet. It Is Smaller in Size Than
Mars Mars is the fourth terrestrial planet. It is smaller in size than Earth and Venus, but larger than Mercury. Of the planets, Mars is the most hospitable to visiting humans, as it has an atmosphere, though it has no oxygen and is very thin. In the early days of the solar system, Mars has had liquid water on its surface, which is proved by the existence of various minerals that require liquid water to form. The current atmosphere of Mars is too thin and cold for liquid water to exist for long periods of times. Still, there is evidence of terrain shaped by flowing liquids, which are probably temporary flows or floods caused by the melting of ice in the ground. Mars has seasons like the Earth, and ice caps at the poles that grow and shrink over the course of the year. They consist of water ice and CO2 ice, the latter varying more with the seasons. One year on Mars is a bit less than two Earth years. Mars has two moons, Phobos and Deimos. They are very small compared to Mars, and are likely to be asteroids captured by Mars's gravity in the distant past. Giant planets and their moons The outer four planets of the solar system are known as the giant planets, because of their large size (compared to the terrestrial planets). The giant planets of our solar system can be further divided into two categories: gas giants (Jupiter and Saturn) and ice giants (Uranus and Neptune). The gas giants consist mainly of hydrogen (up to 90%) and helium, while the ice giants are mostly "ices" such as water and ammonia, with only some 20% of hydrogen.
[Show full text]
Comparative Habitability of Transiting Exoplanets
Draft version October 1, 2015 A Preprint typeset using LTEX style emulateapj v. 04/17/13 COMPARATIVE HABITABILITY OF TRANSITING EXOPLANETS Rory Barnes1,2,3, Victoria S. Meadows1,2, Nicole Evans1,2 Draft version October 1, 2015 ABSTRACT Exoplanet habitability is traditionally assessed by comparing a planet’s semi-major axis to the location of its host star’s “habitable zone,” the shell around a star for which Earth-like planets can possess liquid surface water. The Kepler space telescope has discovered numerous planet candidates near the habitable zone, and many more are expected from missions such as K2, TESS and PLATO. These candidates often require significant follow-up observations for validation, so prioritizing planets for habitability from transit data has become an important aspect of the search for life in the universe. We propose a method to compare transiting planets for their potential to support life based on transit data, stellar properties and previously reported limits on planetary emitted flux. For a planet in radiative equilibrium, the emitted flux increases with eccentricity, but decreases with albedo. As these parameters are often unconstrained, there is an “eccentricity-albedo degeneracy” for the habitability of transiting exoplanets. Our method mitigates this degeneracy, includes a penalty for large-radius planets, uses terrestrial mass-radius relationships, and, when available, constraints on eccentricity to compute a number we call the “habitability index for transiting exoplanets” that represents the relative probability that an exoplanet could support liquid surface water. We calculate it for Kepler Objects of Interest and find that planets that receive between 60–90% of the Earth’s incident radiation, assuming circular orbits, are most likely to be habitable.
[Show full text]
Dynamical Evolution and Bombardment of the Early Solar System: a Few Highlights from the Last 50 Years
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1545.pdf DYNAMICAL EVOLUTION AND BOMBARDMENT OF THE EARLY SOLAR SYSTEM: A FEW HIGHLIGHTS FROM THE LAST 50 YEARS. W. F. Bottke1 1Southwest Research Institute and NASA’s SSERVI-ISET Team, Boulder, CO ([email protected]). Introduction. Over the last several decades, there orbital migration of Jupiter and Saturn in a gas disk, has been a transformation in our theoretical under- Jupiter could have migrated inward all the way to ~1.5 standing of early Solar System evolution. Historically, AU from the Sun. At that point Jupiter and Saturn it was thought that the planets and small bodies formed could have become trapped in their mutual 2:3 reso- near their current locations. Starting in the 1980’s with nance and would have begun to move outward. pioneering work by Ward, Lin, and Papaloizou, (for The Grand Tack model studied the gravitational planet–gas disk interactions) in the late 1970s and Fer- scattering of asteroids by Jupiter and Saturn during nandez and Ip (for planet–planetesimal disk interac- their inward, then outward migration. This model not tions) in the early 1980s, however, it has now become only reproduces the mass and mixture of spectral types clear that the structure of the Solar System most likely in the asteroid belt, but also truncates the planetesimal changed as the planets grew and migrated [e.g., 1, 2]. disk from which the terrestrial planets form, as in Han- Evidence for giant planet migration can be found in sen’s work. This allowed them to form a low-mass the orbital structures of the Kuiper belt, Trojans, irreg- Mars.
[Show full text]
Terrestrial Planets in High-Mass Disks Without Gas Giants
A&A 557, A42 (2013) Astronomy DOI: 10.1051/0004-6361/201321304 & c ESO 2013 Astrophysics Terrestrial planets in high-mass disks without gas giants G. C. de Elía, O. M. Guilera, and A. Brunini Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata and Instituto de Astrofísica de La Plata, CCT La Plata-CONICET-UNLP, Paseo del Bosque S/N, 1900 La Plata, Argentina e-mail: [email protected] Received 15 February 2013 / Accepted 24 May 2013 ABSTRACT Context. Observational and theoretical studies suggest that planetary systems consisting only of rocky planets are probably the most common in the Universe. Aims. We study the potential habitability of planets formed in high-mass disks without gas giants around solar-type stars. These systems are interesting because they are likely to harbor super-Earths or Neptune-mass planets on wide orbits, which one should be able to detect with the microlensing technique. Methods. First, a semi-analytical model was used to deﬁne the mass of the protoplanetary disks that produce Earth-like planets, super- Earths, or mini-Neptunes, but not gas giants. Using mean values for the parameters that describe a disk and its evolution, we infer that disks with masses lower than 0.15 M are unable to form gas giants. Then, that semi-analytical model was used to describe the evolution of embryos and planetesimals during the gaseous phase for a given disk. Thus, initial conditions were obtained to perform N-body simulations of planetary accretion. We studied disks of 0.1, 0.125, and 0.15 M.
[Show full text]
Symposium on Telescope Science
Proceedings for the 26th Annual Conference of the Society for Astronomical Sciences Symposium on Telescope Science Editors: Brian D. Warner Jerry Foote David A. Kenyon Dale Mais May 22-24, 2007 Northwoods Resort, Big Bear Lake, CA Reprints of Papers Distribution of reprints of papers by any author of a given paper, either before or after the publication of the proceedings is allowed under the following guidelines. 1. The copyright remains with the author(s). 2. Under no circumstances may anyone other than the author(s) of a paper distribute a reprint without the express written permission of all author(s) of the paper. 3. Limited excerpts may be used in a review of the reprint as long as the inclusion of the excerpts is NOT used to make or imply an endorsement by the Society for Astronomical Sciences of any product or service. Notice The preceding “Reprint of Papers” supersedes the one that appeared in the original print version Disclaimer The acceptance of a paper for the SAS proceedings can not be used to imply or infer an endorsement by the Society for Astronomical Sciences of any product, service, or method mentioned in the paper. Published by the Society for Astronomical Sciences, Inc. First printed: May 2007 ISBN: 0-9714693-6-9 Table of Contents Table of Contents PREFACE 7 CONFERENCE SPONSORS 9 Submitted Papers THE OLIN EGGEN PROJECT ARNE HENDEN 13 AMATEUR AND PROFESSIONAL ASTRONOMER COLLABORATION EXOPLANET RESEARCH PROGRAMS AND TECHNIQUES RON BISSINGER 17 EXOPLANET OBSERVING TIPS BRUCE L. GARY 23 STUDY OF CEPHEID VARIABLES AS A JOINT SPECTROSCOPY PROJECT THOMAS C.
[Show full text]
Formation of Telluric Planets and the Origin of Terrestrial Water
BIO Web of Conferences 2, 01003 (2014) DOI: 10.1051/bioconf/20140201003 C Owned by the authors, published by EDP Sciences, 2014 Formation of telluric planets and the origin of terrestrial water Sean Raymond1;a 1Laboratoire d’Astrophysique de Bordeaux, UMR 5804 Abstract. Simulations of planet formation have failed to reproduce Mars’ small mass (compared with Earth) for 20 years. Here I will present a solution to the Mars problem that invokes large-scale migration of Jupiter and Saturn while they were still embedded in the gaseous protoplanetary disk. Jupiter first migrated inward, then "tacked" and migrated back outward when Saturn caught up to it and became trapped in resonance. If this tack occurred when Jupiter was at 1.5 AU then the inner disk of rocky planetesimals and em- bryos is truncated and the masses and orbits of all four terrestrial planet are quantitatively reproduced. As the giant planets migrate back outward they re-populate the asteroid belt from two different source populations, matching the structure of the current belt. C-type material is also scattered inward to the terrestrial planet-forming zone, delivering about the right amount of water to Earth on 10-50 Myr timescales. 1 Introduction 2 The formation of terrestrial planets As described in the Introduction, the final stages of terrestrial planet formation take place in the presence of any giant planets that may have formed. In addition, it is during this phase that bodies are large enough that during gravitational close encounters they can obtain large eccentricities. Thus, the feeding zones of the terrestrial planets are determined during their final accretion.
[Show full text]
Arxiv:2106.07648V1 [Astro-Ph.EP] 14 Jun 2021 Behaviors from Periodic, E.G., Kepler-1520 B (Rappaport Et Al
Draft version June 16, 2021 Typeset using LATEX default style in AASTeX62 LBT Reveals Large Dust Particles and a High Mass Loss Rate for K2-22 b Everett Schlawin,1 Kate Y. L. Su,1 Terry Herter,2 Andrew Ridden-Harper,2, 3 and Daniel´ Apai1, 4 1Steward Observatory The University of Arizona 933 North Cherry Avenue Tucson, AZ 85721, USA 2Astronomy Department Cornell University Ithaca NY 14853 3Carl Sagan Institute Cornell University Ithaca NY 14853 4Lunar and Planetary Laboratory The University of Arizona 1629 E. University Blvd. Tucson, AZ 85721, USA ABSTRACT The disintegrating planet candidate K2-22 b shows periodic and stochastic transits best explained by an escaping debris cloud. However, the mechanism that creates the debris cloud is unknown. The grain size of the debris as well as its sublimation rate can be helpful in understanding the environment that disintegrates the planet. Here, we present simultaneous photometry with the g band at 0.48 µm and KS band at 2.1 µm using the Large Binocular Telescope. During an event with very low dust activity, we put a new upper limit on the size of the planet of 0.71 R⊕ or 4500 km. We also detected a medium-depth transit which can be used to constrain the dust particle sizes. We ﬁnd that the median particle size must be larger than about 0.5 to 1.0 µm, depending on the composition of the debris. This leads to a high mass loss rate of about 3 × 108 kg/s that is consistent with hydrodynamic escape models.
[Show full text]
A Seminar Named: EARTH 2.0
Syrian Arabic Republic Ministry of Education National Center for the Distinguished` A Seminar Named: EARTH 2.0 Presented by: Amir Najjar Supervised by: Ms. Wafaa 11th grade 2015-2016 0 Contents Introduction:............................................................................... 2 Kepler Spacecraft and its mission: ............................................. 3 The spacecraft's specifications: ............................................... 3 Camera: .................................................................................... 3 Primary Mirror: ........................................................................ 4 Communications: ..................................................................... 4 Kepler’s Story: .......................................................................... 4 Kepler-452b: ............................................ 8 Conclusion: .............................................. 9 References: ............................................ 11 1 Introduction: -Is it true that we are finding new planets that are similar to Earth’s specifications? -Is it possible to live there? -What is the famous spacecraft that is finding such planets? -Who is Earth’s Older Cousin? Can we move and live there? -Is this planet larger or smaller than Earth? Is its distance from its star the same as the distance between Earth and Sun? -Are there any forms of life on this planet? Or we could implant forms of life in this planet? -Is this planet a rocky world in the first place? -We’re going to discuss all this in
[Show full text]
Physical Geology
Chapter 22 The Origin of Earth and the Solar System Learning Objectives After carefully reading this chapter, completing the exercises within it, and answering the questions at the end, you should be able to: • Describe what happened during the big bang, and explain how we know it happened • Explain how clouds of gas floating in space can turn into stars, planets, and solar systems • Describe the types of objects that are present in our solar system, and why they exist where they do • Outline the early stages in Earth’s history, including how it developed its layered structure, and where its water and atmosphere came from • Explain how the Moon formed, and how we know • Summarize the progress so far in the hunt for habitable-zone planets outside of our solar system • Explain why the planetary systems we have discovered so far raise questions about our model of how the solar system formed The story of how Earth came to be is a fascinating contradiction. On the one hand, many, many things had to go just right for Earth to turn out the way it did and develop life. On the other hand, the formation of planets similar to Earth is an entirely predictable consequence of the laws of physics, and it seems to have happened more than once. We will start Earth’s story from the beginning—the very beginning—and learn why generations of stars had to be born and then die explosive deaths before Earth could exist. We will look at what it takes for a star to form, and for objects to form around it, as well as why the nature of those objects depends on how far away from the central star they form.
[Show full text]
Kepler Spies Most Earth-Like Planet Yet NASA Mission Finds a Potentially Rocky World Orbiting a Star That Resembles the Sun
IN FOCUS NEWS The programme will also provide valuable edges, where the ice tends to be warmer, thicker the coast to track large-scale ice loss over five information on the physical characteristics of and full of crevices. “It’s still a challenge to get years. Analysing that ice loss in light of the new glacier ice. Last December, geophysicist Beata the mass of these glaciers,” she says. topographical and oceanographic data will help Csatho of the University at Buffalo in New York When the aerial phase of OMG begins next researchers to determine where, and to what and her colleagues reported using surface- year, planes will fly inland from the coast, taking extent, deeper saltwater currents affect glaciers. elevation data to estimate how much ice mass measurements of slight changes in gravitational Lipscomb says that all these OMG data Greenland had lost between 1993 and 2012 pull that can be used to produce low-resolution should help modellers as they incorporate (B. M. Csatho et al. Proc. Natl Acad. Sci. USA maps of the topography under both water and ocean–ice interactions around Greenland 111, 18478–18483; 2014). The data were fairly ice. Planes will also drop more than 200 temper- into their models. That work is still in its early reliable over the island’s interior, Csatho says, ature and salinity probes into fjords and coastal stages, he says, “but the data that they are get- but measurements were more difficult along its waters, and take radar measurements along ting in this project is exactly what we need”.
[Show full text]
The Impact of Planetary Rotation Rate on the Reflectance and Thermal Emission Spectrum of Terrestrial Exoplanets Around Sun-Like Stars
The Impact of Planetary Rotation Rate on the Reflectance and Thermal Emission Spectrum of Terrestrial Exoplanets Around Sun-like Stars Scott D. Guzewich1,2 (301-286-1542), Jacob Lustig-Yaeger3,4, Christopher Evan Davis3,4, Ravi Kumar Kopparapu1,2,4, Michael J. Way5, Victoria S. Meadows3,4 1NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771 2Sellers Exoplanet Environments Collaboration, NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771 3University of Washington, Department of Astronomy, Box 951580, Seattle, WA 98195 4NASA NExSS Virtual Planetary Laboratory, Box 951580, Seattle, WA 98195 5NASA Goddard Institute for Space Studies, 2880 Broadway, New York, NY 10025 ABSTRACT Robust atmospheric and radiative transfer modeling will be required to properly interpret reflected light and thermal emission spectra of terrestrial exoplanets. This will help break observational degeneracies between the numerous atmospheric, planetary, and stellar factors that drive planetary climate. Here we simulate the climates of Earth-like worlds around the Sun with increasingly slow rotation periods, from Earth-like to fully Sun-synchronous, using the ROCKE-3D general circulation model. We then provide these results as input to the Spectral Planet Model (SPM), which employs the SMART radiative transfer model to simulate the spectra of a planet as it would be observed from a future space-based telescope. We find that the primary observable effects of slowing planetary rotation rate are the altered cloud distributions, altitudes, and opacities which subsequently drive many changes to the spectra by altering the absorption band depths of biologically-relevant gas species (e.g., H2O, O2, and O3).
[Show full text]
Rest of the Solar System” As We Have Covered It in MMM Through the Years
As The Moon, Mars, and Asteroids each have their own dedicated theme issues, this one is about the “rest of the Solar System” as we have covered it in MMM through the years. Not yet having ventured beyond the Moon, and not yet having begun to develop and use space resources, these articles are speculative, but we trust, well-grounded and eventually feasible. Included are articles about the inner “terrestrial” planets: Mercury and Venus. As the gas giants Jupiter, Saturn, Uranus, and Neptune are not in general human targets in themselves, most articles about destinations in the outer system deal with major satellites: Jupiter’s Io, Europa, Ganymede, and Callisto. Saturn’s Titan and Iapetus, Neptune’s Triton. We also include past articles on “Space Settlements.” Europa with its ice-covered global ocean has fascinated many - will we one day have a base there? Will some of our descendants one day live in space, not on planetary surfaces? Or, above Venus’ clouds? CHRONOLOGICAL INDEX; MMM THEMES: OUR SOLAR SYSTEM MMM # 11 - Space Oases & Lunar Culture: Space Settlement Quiz Space Oases: Part 1 First Locations; Part 2: Internal Bearings Part 3: the Moon, and Diferent Drums MMM #12 Space Oases Pioneers Quiz; Space Oases Part 4: Static Design Traps Space Oases Part 5: A Biodynamic Masterplan: The Triple Helix MMM #13 Space Oases Artiﬁcial Gravity Quiz Space Oases Part 6: Baby Steps with Artiﬁcial Gravity MMM #37 Should the Sun have a Name? MMM #56 Naming the Seas of Space MMM #57 Space Colonies: Re-dreaming and Redrafting the Vision: Xities in
[Show full text]