1 Open Research Online The Open University s repository of research publications and other research outputs Jupiter friend or foe? II: the Centaurs Journal Article How to cite: Horner, J. and Jones, B. W. (2009). Jupiter friend or foe? II: the Centaurs. International Journal of Astrobiology, 8(2) pp For guidance on citations see FAQs. c 2009 Cambridge University Press Version: Version of Record Link(s) to article on publisher s website: Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online s data policy on reuse of materials please consult the policies page. oro.open.ac.uk
2 International Journal of Astrobiology 8 (2): (2009) Printed in the United Kingdom doi: /s f Cambridge University Press Jupiter friend or foe? II: the Centaurs Astronomy Group, Physics & Astronomy, The Open University, Milton Keynes MK7 6AA, UK Abstract: It has long been assumed that the planet Jupiter acts as a giant shield, significantly lowering the impact rate of minor bodies upon the Earth, and thus enabling the development and evolution of life in a collisional environment which is not overly hostile. In other words, it is thought that, thanks to Jupiter, mass extinctions have been sufficiently infrequent that the biosphere has been able to diversify and prosper. However, in the past, little work has been carried out to examine the validity of this idea. In the second of a series of papers, we examine the degree to which the impact risk resulting from objects on Centaur-like orbits is affected by the presence of a giant planet, in an attempt to fully understand the impact regime under which life on Earth has developed. The Centaurs are a population of ice-rich bodies which move on dynamically unstable orbits in the outer Solar system. The largest Centaurs known are several hundred kilometres in diameter, and it is certain that a great number of kilometre or sub-kilometre sized Centaurs still await discovery. These objects move on orbits which bring them closer to the Sun than Neptune, although they remain beyond the orbit of Jupiter at all times, and have their origins in the vast reservoir of debris known as the Edgeworth Kuiper belt that extends beyond Neptune. Over time, the giant planets perturb the Centaurs, sending a significant fraction into the inner Solar System where they become visible as short-period comets. In this work, we obtain results which show that the presence of a giant planet can act to significantly change the impact rate of short-period comets on the Earth, and that such planets often actually increase the impact flux greatly over that which would be expected were a giant planet not present. Received 31 July 2008, accepted 20 October 2008, first published online 24 December 2008 Key words: Centaurs, comets general, minor planets, planets and satellites general, Solar System formation, Solar System general. Introduction In our previous paper, Jupiter friend or foe? I: the asteroids (Horner & Jones 2008, Paper I), we highlighted the idea that Jupiter has significantly reduced the impact rate on the Earth of minor bodies, notably small asteroids and comets, thereby allowing the biosphere to survive and develop (for example, see Greaves 2006). This idea is widely accepted, both in the scientific community and beyond. It is clearly the case that a sufficiently high rate of large impacts would result in the evolution of a biosphere being stunted by frequent mass extinctions, each bordering on global sterilization. Were Jupiter not present in our Solar System, it is argued, such frequent mass extinctions would occur on the Earth, and therefore the development of life would be prevented. We also pointed out that, until recently, very little work had been carried out to examine the effects of giant planets on the flux of minor bodies through the inner Solar System. Wetherill (1994) showed that in systems containing bodies that grew only to the size of, say, Uranus and Neptune, the impact flux from comets originating in the Oort Cloud 1, experienced by any terrestrial planet, would be a factor of a thousand times greater than that seen today in our System, as a direct result of less efficient ejection of material from the System during its early days. This work is discussed in more detail in Paper I, which also outlines recent work by Laasko et al. (2006), who conclude that Jupiter in its current orbit, may provide a minimal of protection to the Earth. Paper I also mentions the work of Gomes et al. (2005), from which it is clear that removing Jupiter from our Solar System would result in far fewer impacts on the Earth by lessening, or removing entirely, the effects of the Late Heavy Bombardment in the inner Solar System. Thus, it seems that the idea of Jupiter, the protector dates back to the time when the main impact risk to the Earth was thought to arise from the Oort cloud comets (Wetherill 1994). Many such objects are actually expelled from the Solar 1 The Oort cloud is a vast shell of icy bodies, centred on the Sun, extending to approximately halfway to the nearest star (some 10 5 AU). Bodies swung inwards from this cloud typically have orbital periods of tens of thousands, or even millions of years, and are often described as long-period comets.
3 76 System after their first pass through its inner reaches, as a result of Jovian perturbations, which clearly lowers the chance of one of these cosmic bullets striking the Earth (see, for example, Matese & Lissauer 2004). Recently, however, it has become accepted that near-earth objects (primarily asteroids, with a contribution from the short-period comets 2 ) pose a far greater threat to the Earth. Indeed, it has been suggested that the total cometary contribution to the impact hazard may be no higher than 25% (Chapman & Morrison 1994). In order to study the relationship between a giant planet and the impact rate on a terrestrial world, we are running n-body simulations to see how varying the mass of Jupiter would change the impact rate on Earth. Since there are three source populations that provide the main impact threat, the asteroids, the short-period comets, and the Oort cloud comets, we are examining each population in turn. In Paper I we examined the effect of changing Jupiter s mass on the impact rate experienced by the Earth from objects flung inwards from the asteroid belt. Our results were surprising. At very low and very high Jupiter masses, the impact rate was particularly low. However, there was a sharp peak in the impact flux at around 0.20 times the mass of our Jupiter, at which point the Earth in our simulations experienced almost twice as many impacts as it did in the simulation of our own Solar System. This shows conclusively that the idea of Jupiter the shield is far from a complete description of how giant planets affect terrestrial impact fluxes, and that more work is needed to examine the problem. In this paper, we detail our results for the short-period comets. The main source of these objects is the Centaurs, a transient population of ice-rich bodies ranging up to a few hundred kilometres across. They orbit with perihelia between the orbits of Jupiter and Neptune, and are themselves sourced from the region just beyond the orbit of Neptune, where the Edgeworth Kuiper belt and the Scattered Disk objects lie (Levison & Duncan 1997; Horner et al. 2004). The giant planets perturb the Centaurs, and send a significant fraction into the inner Solar System, where they become visible as short-period comets. Our results for Oort cloud comets (the reservoir studied by Wetherill) will be detailed in later work. Simulations Of the three parent populations for Earth-impacting bodies, the simplest to model are the short-period comets. However, given that we wished to look at the effects of Jupiter on the impact flux, taking a population that has already been significantly perturbed by the giant planet would clearly have been a mistake. Instead, we chose to use the Centaurs to provide our population of potentially threatening objects. 2 Short-period comets typically have orbital periods significantly less than 200 years. In contrast to the long-period comets, the great majority of these objects originate from the Edgeworth Kuiper Belt (which stretches out to around 20 AU beyond the orbit of Neptune), and from the associated Scattered Disk. In order to create a swarm of test objects that might evolve onto Earth-impacting orbits, we searched the Centaur and Trans-Neptunian ( Beyond Neptune ) object lists hosted by the Minor Planet Center (MPC) for all objects with perihelia between 17 and 30 AU (see, for example, harvard.edu/iau/lists/centaurs.html, harvard. edu/iau/lists/tnos.html). This gave a total of 105 objects, including Pluto. Pluto was removed, giving a sample of 104 objects. These were then cloned 1029 times each, with each orbit obtained from the MPC acting as the central point in a 7r7r7r3 grid in a-e-i-v space (with clones separated by 0.1 AU in semi-major axis, 0.05 in eccentricity, 0.5 degrees in inclination, and 5 degrees in the argument of perihelion). The steps used, and the number of clones created in a given element, were chosen to disperse the clones widely enough in orbital element space around the parent so that rapid dynamical dispersion would occur. In addition, it is clear that our initial sample of 104 objects contains a number of bodies on stable orbits (in mean-motion resonances, for example). Given that we are interested in the behaviour of those objects in the outer Solar System which have already left the stable reservoirs, it was important that the cloning process could move many of the clones of these objects onto less stable orbits, allowing them to diffuse through the Solar System within the period of our integrations. The cloning process produced a population of just over objects covering a wide range of values in orbital element space, orbits which were simulated for a period of 10 million years using the hybrid integrator contained within the MERCURY package (Chambers 1999), with an integration time step of 120 days, along with the planets Earth, Jupiter, Saturn, Uranus and Neptune, all with initial orbital elements equal to their present values (although they barely changed during the simulation). The integration length was chosen to provide a balance between required computation time and the statistical significance of the results obtained. In the simulation the cloned objects were treated as massless particles, feeling the gravitational pull of the planets and the Sun, but experiencing no interaction with one another. The massive bodies (the planets), in turn, experienced no perturbation from the massless particles, but were able to fully interact with one another. As in Paper I, the Earth within our simulations was inflated to have a radius of one million kilometres, in order to enhance the impact rate from objects on Earth crossing orbits. Simple initial integrations were again carried out to confirm that this inflation did affect the impact rate as expected, with the flux scaling as expected with the cross-sectional area of the planet. In order to examine the effect of Jovian mass on the impact rate, we ran thirteen separate scenarios. In the first, we used a Jupiter with the same mass as that in our Solar System (so one Jupiter mass), while in the others, planets of mass 0.01, 0.05, 0.10, 0.15, 0.20, 0.25, 0.30, 0.50, 0.75, 1.50 and 2.00 times the mass of the present Jupiter were substituted in its place. Finally, a run was carried out in which no Jupiter was present. Hereafter, we refer to these runs by the mass of the planet used, so that, for example, M 1.00 refers to
4 Jupiter friend or foe? II: the Centaurs 77 the run using a planet of one Jupiter mass, and M 0.01 refers to the run using a planet of 0.01 Jupiter masses. The (initial) orbital elements of Jupiter, together with all the other planets, were identical in all cases. However, in reality, if our Solar System had formed with a Jupiter of different mass, the architecture of the outer Solar System would probably be somewhat different. Rather than try to quantify the uncertain effects of a change to the configuration of our own Solar System, we felt it best to change solely the mass of the Jupiter in our work, and therefore work with a known, albeit modified, system, rather than a theoretical construct. For a flux of objects moving inwards from the Edgeworth Kuiper belt, this does not seem unreasonable by choosing a population of objects well beyond the Jupiter in our simulations, with initial perihelia between 17 and 30 AU, we have greatly reduced the planet s influence on the objects prior to the start of our simulations, and believe this method allows us to make a fair assessment of the role of Jovian mass on such objects. The complete suite of integrations ran for some nine months of real time, spread over the cluster of machines sited at the Open University. This nine months of real time equates to over 12 years of computation time, and resulted in measures of the impact flux for each of the 13 Jupiters. Further, the eventual fate of each object was followed, allowing the determination of the dynamical half-life of the population in the different runs. With the constant trickle of objects being lost by ejection or collision with the Sun or with planets other than the Earth, this half-life is clearly an important factor in determining the threat posed, since a more stable population (one with a longer half-life), with the same parent-flux, would lead to an enhanced population of impactors, reducing any shielding effect resulting from the lowered impact rate per simulated object. Note that objects placed on Earth-crossing orbits will devolatilize on a time scale orders of magnitude shorter than the 10 Myr of our integrations. Comets are observed to fragment or disintegrate during their lifetimes with some regularity (a famous example of such disintegration being comet 3D/Biela, which is discussed in some length in Babadzhanov et al. (1991)). However, it seems likely that many comets simply age and switch off, becoming husks that resemble asteroidal bodies (Levison et al. 2006). It is unlikely, then, that the effects of de-volatilization will alter the main thrust of our results, even though objects travelling inward from orbits with initial perihelia beyond about 17 AU can remain in the inner Solar System for periods significantly longer than the theoretical de-volatilization time (Horner & Evans 2004). Results As can be seen from Fig. 1, the rate at which objects hit the Earth clearly ranges widely as a function of the mass of the Jupiter-like planet in each simulation. The run without a Jupiter (M 0.00 ), shown in red on the upper left-hand panel, clearly displays a much slower start to the impacts than the runs involving higher-mass planets (upper right-hand plot). This is a result of the fact that, with no Jupiter to nudge things our way, the bulk of the work is done by Saturn, which, being both smaller and further away from the Earth, has a much harder time injecting Earth-crossers. The third column in Table 1 gives N ejected the total number of objects that were removed during the course of the simulations. In our runs, objects were destroyed either on impact with one of the massive bodies (the Sun, Earth, Jupiter, Saturn, Uranus and Neptune), or on reaching a distance of 1000 AU from the central body. Unlike the figure showing the impact rate on Earth, it is clear from the tabulated data that the rate at which the objects are removed from the Solar System increases with the mass of Jupiter. The value of N ejected has been adjusted to take account of the fact that, in each of the runs, 883 of the initial population of objects were placed on orbits so eccentric that they reached the 1000 AU ejection distance on their first orbit. These have been removed from the total in each case, and the value of the dynamical half-life, T 1/2, has been calculated from this modified value T 1/2 is obtained for the corrected population of objects in each simulation, in Myr. The total number of particles used in the calculation has, similarly, been modified, so that T 1/2 represents that of the 99.9% of our population that started the simulation on bound orbits. One thing that is immediately obvious is that the number of particles removed from the simulations varies far less than the impact flux at Earth, and increases with increasing Jupiter mass. This illustrates the increasing efficiency with which Jupiter flings objects from the Solar System as its mass increases. Given that systems which display longer dynamical halflives would be expected to have a larger steady-state population, the number of impacts, N impact has been scaled by the ratio of T 1/2 of the run in question to that in the M 1.00 case, to give N imp-s. This illustrates the effect that Jupiter has in diminishing the particle population by accelerating their ejection from the system, and gives a more realistic view of the changes in impact flux as a function of Jovian mass. The results of this calculation are given in the final column in Table 1, and plotted in the lower right-hand panel of Fig. 1. Discussion From the results discussed above, it is clear that the notion that any Jupiter would provide more shielding than none at all is incorrect, at least for impactors originating from the population of small objects with initial perihelia in the range AU. It seems that the effect of such a planet on the impact flux on potentially habitable worlds is far more complex than was initially thought. With our current Jupiter, potentially impacting objects are ejected from the system with such rapidity that they pose rather little risk for planets in the habitable zone, and therefore, Jupiter offers a large degree of shielding, compared to smaller versions of the planet. Planets much more massive than Jupiter clearly offer an even higher degree (as can be seen in the M 1.50 and M 2.00 cases). At the other end of the scale, when the Jupiter is of particularly small mass (or when no Jupiter is present), fewer
5 78 Fig. 1. The top two panels show the number of collisions of the simulated objects with the Earth, as a function of time. On the left, we have M 0.00 (red), M 0.01 (cyan), M 0.05 (blue), M 0.10 (green), M 0.15 (black), and M 0.20 (magenta). On the right, we have M 0.25 (black), M 0.30 (magenta), M 0.50 (blue), M 0.75 (green), M 1.00 (cyan), M 1.50 (red) and M 2.00 (yellow). The lower left-hand panel gives the number of impacts as a function of the mass of the Jupiter in the simulation: t=2 Myr (red), 4 Myr (blue), 6 Myr (magenta), 8 Myr (green), 10 Myr (black). Finally, the panel at the lower right shows the number of impacts as a function of the Jupiter mass after ten million years. The solid line and red triangles show the results from our simulations, while the green triangles and dashed line show these numbers adjusted to take account of the variations in the half-life of the ensemble compared to that of the M 1.00 simulation. objects are scattered onto orbits that cross the habitable zone, and so, once again, the impact rate is low. The more interesting situation occurs for intermediate masses, where the giant is massive enough to emplace objects on threatening orbits, but small enough that ejection events are still infrequent. The situation that offers the greatest enhancement to the impact rate is one located around 0.20 M J, in our simulations, at which point the planet is massive enough to efficiently inject objects to Earth-crossing orbits, but small enough that the time spent on these orbits is such that the impact rate is significantly enhanced. The effect of Jupiter on the size of the population of incoming bodies is one that must be considered together with its direct effect on the impact rate from a population of a given size. Given that our various scenarios feature a Solar System like our own, with only the mass of Jupiter changing, it is clear that the inward flux from beyond Neptune would be unchanged between the various scenarios. However, as the mass of Jupiter falls, the efficiency with which the objects are ejected falls, and therefore T 1/2 of that transient population rises. With a longer T 1/2, and the same source flux, the total population at a given time would be larger than for cases with shorter T 1/2, as a steady-state would be reached with more objects moving around the outer Solar System. T 1/2 of our population in the M 0.00 case is 87 million years, compared with a value of 61 Myr in the M 1.00 case, which is readily shown to mean that the true population in the M 0.00 case would be some 40% higher than that in the M 1.00 case. Given that the impact rate should scale linearly with the population of objects, it is clear that this means that the impact rate in the M 0.00 case should be scaled upwards by some 40% to be directly comparable to the M 1.00 case. The results of such calculations are shown in both Fig. 1 and Table 1. In the case of our M 0.00 integrations, 180 simulated objects hit the Earth, compared to 240 collisions in the M 1.00 simulation. If we modify the impact rates as described above, the situation is changed from 181:239 to 259:239. From this we can see that, once one takes into account the increased stability of the object population in the low-mass
6 Jupiter friend or foe? II: the Centaurs 79 Table 1. M is the mass of the Jupiter used in a given run (relative to that of the real Jupiter), N impact is the number of impacts on the Earth over the course of the simulation, while N ejected gives the total number of objects removed from the simulation through either collision (with massive bodies other than the Earth) or ejection. The value of N impact is a corrected value, and ignores the 883 objects that were placed on orbits that led to immediate ejection in the initial population process. T 1/2 gives the dynamical half-life obtained for the corrected population of massless bodies in each simulation, in Myr. N imp-s gives the number of impacts that would be expected from a population enhanced over that described here, as a result of the longer lifetime of the objects in a given system. It is scaled so that the result for the case of our Solar System (M 1.00 ) remains the same M (in M J ) N impact N ejected (in Myr) T 1/2 N imp-s runs, our Jupiter is actually almost equivalently as effective a shield as having none at all, rather than appearing slightly more threatening than the Jupiter-free case. For the higher masses, the half-lives are close enough that the difference in population will be fairly minor, but it is important to keep this population enhancement in mind for the runs with lower Jupiter masses. As the mass of Jupiter decreases towards that of Saturn, 0.30 M J, the relative influence of the planet Saturn in converting Centaurs into short-period comets clearly becomes ever greater. That said, since Saturn is almost twice as far from the Sun as Jupiter, and therefore finds it significantly more difficult to implant objects to Earth-crossing orbits, the simulated Jupiter continues to be the dominant source of such comets down to particularly low masses. At yet smaller masses, approaching that of the planet Mars, M J, one might ask whether we were justified in ignoring the effect of the planet Mars in our simulations. We contend that Mars plays little or no role in the delivery of the great majority of cometary material to the inner Solar System, even in cases where Jupiter is not present. Without Jupiter, Saturn plays the key role in the injection of such bodies Mars is so small that its effect on passing bodies is negligible, and objects placed on Mars-crossing orbits by Jupiter or Saturn are generally far more likely to be moved onto Earth-crossing orbits by one of the giant planets than by their minute sibling. Conclusions As pointed out in Paper I, the idea that the planet Jupiter has acted as an impact shield through the Earth s history is one that is entrenched in planetary science, even though little work has been done to examine this idea. In the second of an ongoing series of studies, we have examined the question of Jovian shielding using a test population of particles on orbits representative of the Centaurs and those trans-neptunian objects with perihelia between 17 and 30 AU, icy bodies that represent the parent population of the short-period comets (through pathways similar to those described in Horner et al. 2003). This is one of three reservoirs of potentially hazardous objects. (Paper I deals with objects sourced from the asteroid belt, and a future paper will deal with comets swung inward from the Oort cloud.) For the studied population, it seems that the Solar System containing our Jupiter is only about as effective in shielding the Earth as a system containing no Jupiter at all. Furthermore, it seems that terrestrial planets in systems containing smaller Jupiters would be subject to a significantly higher rate of impacts than those in systems with planets larger than our own Jupiter. Although our work currently studies systems that differ from our own only in the mass of Jupiter, the broad terms in which it is stated could well apply widely. Only further work will tell, but our initial results already offer intriguing hints as to the true role of giants in the determination of planetary habitability. This work is doubly interesting when considered in concert with the results we obtained in Paper I, which reports the effect of Jupiter on impactors from the asteroid belt. As stated in the Introduction, we found that Jupiters of low and high mass caused fewer impacts than those of intermediate mass (My0.2 M J ), with a similar sharp rise and fall from the impact-maximum to that observed in this paper. In both works, we find that planets of mass similar to, or a bit smaller than, the planet Saturn pose the greatest threat to terrestrial worlds in planetary systems like our own, when placed at Jupiter s current location. For the asteroids, we concluded that this was primarily a result of the depth, breadth and location of the n 6 secular resonance in the main asteroid belt, while for the short-period comets it seems to be down to the interplay between the injection rate of Earth-crossers with the efficiency with which they are then removed from the system. Despite the different causes, the similarity between the shapes of the impact distributions is striking. Future work will continue the study of the role of Jupiter in limiting or enhancing the impact rate on the Earth by examining bodies representative of the Oort cloud (the source of the long-period comets, the population of potential impactors studied by Wetherill in 1994), together with examining the effect of Jovian location on the impact fluxes engendered by the three populations. Given the surprising outcome of our work to date, we hesitate to anticipate future outcomes. Additionally, future work will also consider whether the absence of a Jupiter-like body would change the populations
7 80 of objects that reside in the reservoirs that provide the bulk of the impact hazard, a possible effect ignored in this work. Acknowledgements This work was carried out with funding from STFC, and JH and BWJ gratefully acknowledge the financial support given by that body. References Babadzhanov, P.B., Wu, Z., Williams, I.P. & Hughes, D.W. (1991). The Leonids, Comet Biela and Biela s associated meteor stream. Mon. Not. R. Astron. Soc. 253, Chambers, J.E. (1999). A hybrid symplectic integrator that permits close encounters between massive bodies. Mon. Not. R. Astron. Soc. 304, Chapman, C.R. & Morrison, D. (1994). Impacts on the Earth by asteroids and comets: assessing the hazard. Nature 367, Greaves, J.S. (2006). Persistent hazardous environments around stars older than the Sun. Int. J. Astrobiology 5, Gomes, R., Levison, H.F., Tsiganis, K. & Morbidelli, A. (2005). Origin of the cataclysmic Late Heavy Bombardment period of the terrestrial planets. Nature 435, Horner, J., Evans, N.W. & Bailey, M.E. (2004). Simulations of the population of Centaurs I. The bulk statistics. Mon. Not. R. Astron. Soc. 354, Horner, J., Evans, N.W., Bailey, M.E. & Asher, D.J. (2003). The populations of comet-like bodies in the Solar system. Mon. Not. R. Astron. Soc. 343, Horner, J. & Jones, B.W. (2008). Jupiter friend or foe? I: the asteroids. Int. J. Astrobiology 7(3 4), Laasko, T., Rantala, J. & Kaasalainen, M. (2006). Gravitational scattering by giant planets. Astron. Astrophys. 456, Levison, H.F. & Duncan, M.J. (1997). From the Kuiper Belt to Jupiterfamily comets: the spatial distribution of ecliptic comets. Icarus 127, Levison, H.F., Terrell, D., Wiegert, P.A., Dones, L. & Duncan, M.J. (2006). On the origin of the unusual orbit of comet 2P/Encke. Icarus 182, Matese, J.J. & Lissauer, J.J. (2004). Perihelion evolution of observed new comets implies the dominance of the galactic tide in making Oort cloud comets discernable. Icarus 170, Wetherill, G.W. (1994). Possible consequences of absence of Jupiters in planetary systems. Astrophys. Space Sci. 212,
Jupiter friend or foe? I: the asteroids J. Horner and B. W. JONES Astronomy Group, Physics & Astronomy, The Open University, Milton Keynes, MK7 6AA, UK e-mail: email@example.com Phone: +44 1908 653229
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Our Planetary System Earth, as viewed by the Voyager spacecraft 7.1 Studying the Solar System Our goals for learning: What does the solar system look like? What can we learn by comparing the planets to
The Solar System What is the solar system? It is our Sun and everything that travels around it. Our solar system is elliptical in shape. That means it is shaped like an egg. Earth s orbit is nearly circular.
7. Our Solar System Terrestrial & Jovian planets Seven large satellites [moons] Chemical composition of the planets Asteroids & comets The Terrestrial & Jovian Planets Four small terrestrial planets Like
Chapter 6 Formation of Planetary Systems: Our Solar System and Beyond What does the solar system look like? The solar system exhibits clear patterns of composition and motion. These patterns are far more
Monografías de la Real Academia de Ciencias de Zaragoza. 25: 115 120, (2004). Extra-solar massive planets with small semi-major axes? S. Fernández, D. Giuliodori and M. A. Nicotra Observatorio Astronómico.
Announcement Chapter 12 Asteroids, Comets, and Dwarf Planets Mastering astronomy assignment 11 Due May 11, 8 am Read Chapters 12 and 13 Two Types of Solar System Debris Comet-Asteroid Similarities Size
Astronomy 110: SURVEY OF ASTRONOMY 4. Formation of Solar Systems 1. A Survey of the Solar System 2. The Solar System s Early History 3. Other Planetary Systems The solar system s rich and varied structure
Exercises 131 The Falling Apple (page 233) 1 Describe the legend of Newton s discovery that gravity extends throughout the universe According to legend, Newton saw an apple fall from a tree and realized
Solar System Overview Planets: Four inner planets, Terrestrial planets Four outer planets, Jovian planets Asteroids: Minor planets (planetesimals) Meteroids: Chucks of rocks (smaller than asteroids) (Mercury,
Formation of the Solar System (Chapter 8) Based on Chapter 8 This material will be useful for understanding Chapters 9, 10, 11, 12, 13, and 14 on Formation of the solar system, Planetary geology, Planetary
Introduction to the Solar System Lesson Objectives Describe some early ideas about our solar system. Name the planets, and describe their motion around the Sun. Explain how the solar system formed. Introduction
The long-term stability of planetary systems Long-term stability of planetary systems The problem: A point mass is surrounded by N > 1 much smaller masses on nearly circular, nearly coplanar orbits. Is
Cosmic Journey: A Solar System Adventure General Information Imagine it a huge spiral galaxy containing hundreds of billions of stars, spiraling out from a galactic center. Nestled deep within one of the
Giant Molecular Clouds http://www.astro.ncu.edu.tw/irlab/projects/project.htm Galactic Open Clusters Galactic Structure GMCs The Solar System and its Place in the Galaxy In Encyclopedia of the Solar System
Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Our Solar System is a collection of gravitationally interacting bodies that include Earth and the Moon. Universal
Chapter 8 Welcome to the Solar System 8.1 The Search for Origins What properties of our solar system must a formation theory explain? What theory best explains the features of our solar system? What properties
Teacher Information Background Information Students will learn about the Solar System while practicing communication skills. Materials clipboard for each student pencils copies of map and Available Destinations
How did the Solar System form? Is our solar system unique? Are there other Earth-like planets, or are we a fluke? Under what conditions can Earth-like planets form? Is life common or rare? Ways to Find
CHAPTER 4 A Family of Planets SECTION 4 Moons BEFORE YOU READ After you read this section, you should be able to answer these questions: How did Earth s moon probably form? How does the moon s appearance
Chapter 7 Our Planetary System Agenda Pass back & discuss Test 2 Where we are (at) Ch. 7 Our Planetary System Finish Einstein s Big Idea Earth, as viewed by the Voyager spacecraft A. General Basics Intro
NOTES: GEORGIA HIGH SCHOOL SCIENCE TEST THE SOLAR SYSTEM 1.What is a Solar system? A solar system consists of: * one central star, the Sun and * nine planets: Mercury, Venus, Earth, Mars, Jupiter, Saturn,
Summary: Four Major Features of our Solar System How did the solar system form? According to the nebular theory, our solar system formed from the gravitational collapse of a giant cloud of interstellar
Asteroids, Comets and NEOs Author: Sarah Roberts Asteroids, Comets and NEOs - Introduction Impact craters form when an asteroid, comet or meteorite (which we collectively call impactors ) hits a planet
Chapter 8 Formation of the Solar System Agenda Announce: Mercury Transit Part 2 of Projects due next Thursday Ch. 8 Formation of the Solar System Philip on The Physics of Star Trek Radiometric Dating Lab
Study Guide: Solar System 1. How many planets are there in the solar system? 2. What is the correct order of all the planets in the solar system? 3. Where can a comet be located in the solar system? 4.
LEADER INSTRUCTIONS Toilet Paper Solar System Adapted by Suzanne Chippindale Based on an idea by the late Gerald Mallon, a planetarium educator who spent his life helping students understand the Universe.
Lecture 19: Planet Formation I. Clues from the Solar System 1 Outline The Solar System:! Terrestrial planets! Jovian planets! Asteroid belt, Kuiper belt, Oort cloud Condensation and growth of solid bodies
ASTR 105 The Solar System 1. Orderly motions 2.Two kinds of planets 3.Two kinds of small bodies 4.Exceptions to the rules Today: Group Lab at the end of class Next THURSDAY 03/10: First Group Project Orderly
UC Irvine FOCUS! 5 E Lesson Plan Title: Astronomical Units and The Solar System Grade Level and Course: 8th grade Physical Science Materials: Visual introduction for solar system (slides, video, posters,
Chapter 5. Determining Masses of Astronomical Objects One of the most fundamental and important properties of an object is its mass. On Earth we can easily weigh objects, essentially measuring how much
A Solar System Coloring Book Courtesy of the Windows to the Universe Project http://www.windows2universe.org The Sun Size: The Sun is wider than 100 Earths. Temperature: ~27,000,000 F in the center, ~10,000
Summer 2014 Astro 1 Lab Exercise Lab #4: ExoPlanet Detection Wednesday Aug 7,8 and 11 Room 200 in Wilder Lab reports are due by 5 pm on Friday August 15, 2013 Put it in the large ASTRO 1 Lab Box just inside
CHAPTER 3 1 A Solar System Is Born SECTION Formation of the Solar System BEFORE YOU READ After you read this section, you should be able to answer these questions: What is a nebula? How did our solar system
AST 105 HW # Solution Week of September 1 th, 2015 Note: All Problems are from The Cosmic Perspective (6ed) Chapter 6 Review Problems 2. For purposes of astronomy, what advantages does a camera have over
Chapter 6 Formation of Planetary Systems Our Solar System and Beyond The solar system exhibits clear patterns of composition and motion. Sun Over 99.9% of solar system s mass Made mostly of H/He gas (plasma)
Chapter 7 Our Planetary System 7.1 Studying the Solar System Our goals for learning:! What does the solar system look like?! What can we learn by comparing the planets to one another?! What are the major
The Scattered Disk: Origins, Dynamics and End States Rodney S. Gomes Observatório Nacional, Rua General José Cristino 77, CEP 921-, Rio de Janeiro, RJ, Brazil Julio A. Fernández, Tabaré Gallardo Departamento
Space Interactive Internet Scavenger Hunt This interactive internet scavenger hunt is aligned to various space standards. It provides students with an engaging way to learn about planets, the moon, stars,
Name Date Due Date Science 9 Read pages 264-287 of SP to help you answer the following questions: Also, go to a school computer connected to the internet. Go to Mr. Colgur s Webpage at http://sd67.bc.ca/teachers/dcolgur
THE SOLAR SYSTEM - EXERCISES 1 THE SUN AND THE SOLAR SYSTEM Name the planets in their order from the sun. 1 2 3 4 5 6 7 8 The asteroid belt is between and Which planet has the most moons? About how many?
Reading Quiz Clickers The Cosmic Perspective Seventh Edition Our Planetary System 7.1 Studying the Solar System What does the solar system look like? What can we learn by comparing the planets to one another?
Solar System Ages 7+ LER 2891 Grades 2+ Card Game A fun game of thinking & linking! Contents 45 Picture cards 45 Word cards 8 New Link cards 2 Super Link cards Setup Shuffle the two decks together to mix
Imperial College London BSc/MSci EXAMINATION June 2008 This paper is also taken for the relevant Examination for the Associateship SUN, STARS, PLANETS For Second Year Physics Students Wednesday, 4th June
Kinesthetic Solar System Kinesthetic Solar System Demonstration Materials Students Pictures or signs representing each body in the solar system, including comets, and asteroids. Large outside open area,
Bull. Astr. Soc. India (2005) 33, 27 33 Mass limit on Nemesis Varun Bhalerao 1 and M.N. Vahia 2 1 Indian Institute of Technology Bombay, Powai, Mumbai 400 076, India 2 Tata Institute of Fundamental Research,
OUTER PLANETS MINOR MEMBERS OF THE SOLAR SYSTEM SUN Jupiter (Earth for Scale) Jupiter s bands are clouds Hubble view of Jupiter Arrow shows entry point of Galileo probe, Dec. 1995 Galilean moons Io True
SKYTRACK Glossary of Terms Angular distance The angular separation between two objects in the sky as perceived by an observer, measured in angles. The angular separation between two celestial objects in