Near Earth Objects, Our Celestial Neighbors (IAU S236): Opportunity and RiskCambridge University Press, 2007年5月24日 - 500 頁 Near Earth Objects (NEOs), asteroids and comets, are the closest neighbors of the Earth-Moon system. They allow research not yet possible on more distant bodies. The IAU Symposium 236 focused on the specific observation and modeling techniques for NEOs, including radar, exploration by spacecraft, measurement of non-gravitational perturbations; also on the next generation surveys expected to increase a hundred-fold the NEO discovery rate. With data from first generation NEO surveys, we now understand how they formed and evolve, dynamically and physically, opening a window on the universal astrophysical phenomenon of collision, leaving clear markings on the surfaces of planets, including the Earth. NEOs with orbits crossing that of the Earth are also a source of impact risks and potential NEO collisions with the Earth represent a long term threat. Mankind has to put in place a chain of mitigating actions; NEO astronomers have successfully put in place the first link. |
內容
On the Lyapounov exponents of the asteroidal motion subject to resonances | 15 |
Resonant transNeptunian objects as a source of Jupiterfamily comets | 31 |
Migration of comets the terrestrial planets | 55 |
Some aspects of the statistics of nearEarth objects | 69 |
Mostly dormant comets in the NEO population and the meteoroid streams that | 87 |
Properties of meteoroids from different classes of parent bodies | 107 |
Equipment meth | 121 |
Is the nearEarth asteroid 2000 PG3 an extinct comet? | 135 |
Current NEO surveys | 323 |
Spacewatch preparations for the era of deep allsky surveys | 329 |
The next decade of Solar System discovery with PanSTARRS | 341 |
Comprehensive NEO Detection Characterization and Orbits | 353 |
Searching for near Earth objects using Lowell observatorys Discovery Channel | 363 |
NEOrelated scientific and outreach activities at KLENOT | 371 |
Astrometry of small Solar System bodies at the Molėtai observatory | 377 |
Kharkiv study nearEarth asteroids | 385 |
Imaging the NEO population | 151 |
NEA rotations and binaries | 167 |
Physical models of asteroids from sparse photometric data | 191 |
Products | 211 |
Collision and impact simulations including porosity | 223 |
Similarities and discrepancies between Main Belt | 239 |
The power of groundbased midinfrared observations | 261 |
NearEarthobject identification over apparitions using nbody ranging | 281 |
Initial linking methods and their classification | 301 |
The observations of near Earth objects by the automatic mirror astrograph | 391 |
The nature of asteroid Itokawa revealed by Hayabusa | 401 |
Keplerian consequences of an impact on an asteroid and their relevance for a | 417 |
Asteroid mass determination with the Gaia mission | 435 |
Albedo and size of 99942 Apophis from polarimetric observations | 451 |
The IAU role | 467 |
15 years ago now and in the near future | 489 |
常見字詞
2007 International Astronomical albedo angular asteroid astrometric Astron axis binary binary asteroids Binzel bodies bolide Borovička Bottke camera collision cometary comets computed curve deflection density detected diameter distribution dynamical Earth eccentricity ecliptic estimate evolution Figure fireball flux fragmentation G.B. Valsecchi Hayabusa Icarus impact inner cloud International Astronomical Union inversion Itokawa Jedicke Jupiter Kaasalainen lightcurve LSST Lyapunov Lyapunov exponent main belt MBAs meteorites meteoroids method Milani Minor Planet mission Morbidelli motion Muinonen near-Earth asteroids near-Earth objects NEAS NEOS observations Observatory obtained Oort cloud optical orbit determination orbital elements Ostro Pan-STARRS parameters perihelion perihelion distance period perturbations phase angle photometric planetary population Pravec predicted Proceedings IAU Symposium Quadrantids radar region relative resonance rotation Science secular resonances semi-major axis semimajor shape simulations solar system solution space Spacewatch spin surface survey target telescope values vector velocity Vokrouhlický