Mainbelt Asteroids AS3141 Benda Kecil dalam Tata Surya Prodi Astronomi 2007/2008 B. Dermawan.
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Transcript of Mainbelt Asteroids AS3141 Benda Kecil dalam Tata Surya Prodi Astronomi 2007/2008 B. Dermawan.
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Mainbelt Asteroids
AS3141 Benda Kecil dalam Tata SuryaProdi Astronomi 2007/2008
B. Dermawan
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Solar System Formation (1)
• Early stages (a-d)• A lot of steps between d and e• Protoplanetary disk is hot near the Sun
and cold far from the Sun, condensation of gas depending on temperature
• Formation and growth of planetesimals (strongly dependent on relative velocity)
• Formation of terrestrial and giant planets
• Early Jupiter prevents planetesimals growth in its neighborhood origin of asteroids
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Solar System Formation (2)
• Comets originate in the Kuiper-belt at about 40 AU from the Sun
• Long-period comets are scattered into Oort cloud, disturbed and isotropized by the influence of passing stars and the galactic bulge
• Short-period comets go directly from Kuiper-belt to the inner solar system
• Meteorites come from the surfaces of asteroids and from Mars to the Earth. Their measurements in the laboratory has contributed greatly to our knowledge about solar system formation
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Discoveries & Numbering
• Main Belt (Ceres 1801 dwarf planet 2006)• Near-Earth Objects (Eros 1898)• Trojans (Achilles 1906)• Cometary (Hidalgo 1920)• Centaurs (Chiron 1977)
• Trans-Neptunians (Pluto 1930; 1992 QB1 1992)
• Minor planet numbers: (100) in 1868; (1000) in 1923; (10000) in 1999; (100000) in 2005• 25 Oct 07 numbered: 168313, total: 387205
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Topics
Orbits and their evolution Asteroid families Asteroid’s Size Distribution & Collision Mainbelt resonances
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Orbits & Their Evolution
• The vast majority of the asteroids depicted are in the main asteroid belt
• Trojans are shown leading and trailing the position of Jupiter
• Aten, Apollo, and Amor asteroids are seen in the inner solar system, crossing the orbits of Mars and Earth
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Orbits & Their Evolution
Main-belt between 2.1 and 3.3 AU Kirkwood gaps coincide with resonance locations
relative to Jupiter, which may be unstable or stable At inner edge of asteroid belt 6 resonance with
Saturn’s apse rate ~2300 asteroids occupy Jupiter L4 (1242) and L5
(1048) triangular lagrangian points (Trojans), Martian Trojans (1,3), Saturnian Trojans (6,0)
[13 Nov 07] Unstable orbits: Amors (1.017 < q < 1.3), Apollos
(q < 1.017, a > 1), Atens (a < 1), all small objects
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Orbital Elements Time of perihelion
passage, T Semimajor axis, a Eccentricity, e Inclination, i Argument of perihelion, Longitude of ascending
node, ω
Ascending node
Ω Osculating elements and
their epoch Periodic and secular
perturbations
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Proper Elements
Over time spans of ~105 yr a remains on the average constant e and i show periodic oscillations, coupled to
variations of and , respectively (ep,ip) are proper elements
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Histograms 25 Oct 2007
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SDSS Colors of MBAsIvezić et al. 2002
a* 0.89(g-r) + 0.45(r-i) – 0.57
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Asteroid FamiliesSDSS, Ivezić et al. 2002
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Osculating & Proper Orbital Elements
Observed at a particular epoch. Not constant in time caused by gravitational perturbations
Practically constant over tens to hundreds of million of years
a detailed calculation
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Asteroid Family
Objects (fragments) obtained from disruption of a common parent body in a catastrophic collision
~35 % of asteroids in the main-belt are family members
Identification:Identification:• Get some knowledge about the collisional evolution Get some knowledge about the collisional evolution
in the Main-beltin the Main-belt• Obtain information about the internal structure of the Obtain information about the internal structure of the
parent bodyparent body
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Satisfactory Methods
Hierarchical Clustering Method (HCM) (Zappala et al. 1990, 1995) Wavelet Analysis Method (WAM) (Bendjoya et al. 1993, 1997)
Both methods:• Imply ‘heavy’ computational time;• Require ad-hoc parameters or threshold
definitions
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Decomposition
Families
Nesvorný et al. 2005
Background Asteroids
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Terminologies
Cluster: the most prominent groupingClumps: few members but clearly distinct from the
backgroundClans: merge very gradually into the background
density (complex group)Tribes: less statistically significant against the
background Interlopers: temporarily resides in a family/cluster
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Families among MBAs
Families are indicative of collisional process between asteroids aa [au] [au]
sin
sin
ii
0
0.1
0.2
0.3
2.2 2.4 2.6 2.8 3.0 3.2
NysaNysa
VestaVesta
PolanaPolana
CeresCeres
MariaMaria
DoraDora
MassaliaMassalia
AdeonaAdeona
LydiaLydia
ErigoneErigone
LiberatrixLiberatrix
MisaMisa
MerxiaMerxia
VeritasVeritas
AugustaAugusta
RafitaRafita
ChlorisChloris
HenanHenan
NemesisNemesis
ReginitaReginita
NocturnaNocturna
MeliboeaMeliboea
BrasiliaBrasiliaFainaFainaTunicaTunica
JeromeJerome
HestiaHestia
AstridAstrid
BowerBower
TaiyuanTaiyuan
HankoHanko
JunoJuno
HygieaHygiea
VincentinaVincentina
KilopiKilopi
SulamitisSulamitisSimpsonSimpson
AeoliaAeolia
AstaAsta
VibiliaVibilia
TheobaldaTheobalda
CeplechaCeplechaBernesBernes
NaemaNaemaNeleNele
49454945
TsurugistanTsurugistan
LaodicaLaodicaDejaniraDejanira
HoffmeisterHoffmeisterAmnerisAmneris
FloraFlora
ThemisThemis
EunomiaEunomia
KoronisKoronis
EosEos
1981 EO191981 EO19
19811981EO82EO82
1981 UC11981 UC1
1965 SB1965 SB
1985 RU11985 RU1
KarinKarin
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The Age of Asteroid Family Craters counting + production rate (rare visits + unknown constrained factors) Track the orbital evolution of the family members backwards
in time (limited to families < 10 Myr) Compare the evolution model of the size freq. distribution with
observations (poorly unknown some parameters) Deduce from the spin axis distribution of a family (certain special circumstances) Calculate the dispersing time via Yarkovsky thermal forces (unknown initial ejection velocities)
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Asteroid Families
Nesvorný et al. 2005
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Young Asteroid Families
293 Brasilia 80 95 C/X ~50
606 Brangane 30 30 S ~50
Nesvorný et al. 2003
Nesvorný et al. 2005
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Size Distribution & Collisional Evolution
N(R) = N0(R/R0)-, for Rmin < R < Rmax
A population of evolving bodies will at the end arrive at a power law size distribution with = 3.5, provided the collision process is self-similar
= 3.5 implies that most of the mass is in the largest body and most of the surface area in the smallest bodies
Collision:Vesc from Ceres = 0.6 km s-1. Thus, most collisions
are eruptive or destructiveFamilies with similar a, e, and iDust bands
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Asteroid Collision (1)
• Distance traveled in time T: V×T• Volume cut out by the target area: R2×VT• Number of collisions: N = R2VT×n• Average time between collisions:
VnRt
2
1
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Asteroid Collision (2)
Typical relative velocity: V 5 km/s Estimate the Main Belt volume by a donut at
2.5 AU from the Sun with a cross-sectional radius = 0.55 AU volume ~ 51025 km3
Total number of asteroids larger than a given radius R:
R > 1 km ~ 5105
R > 10 km ~ 2103
R > 100 km ~ 35
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Size Distribution
Nine estimates
Davis et al. 2002
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Size Dist. of MBA Families
Shallower slopes than the background
Morbidelli et al. 2003
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Resonance: General Types
Spin-orbit resonance: a commensurability of the rotation period of a satellite with the period of its orbital revolution
Secular resonance: a commensurability of the frequencies of precession of the orientation of orbits (direction of perihelion and of the orbit normal)
Mean motion resonance: the orbital periods of two bodies are close to a ratio of small integers
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Spin-orbit Resonance (1)
o Ex: spin-locked state of the Moon, most natural satellites (Pluto-Charon, Saturn-Titan), binary stellar systems
o 1:1 spin-orbit resonance (synchronous spin state)o For a non-spherically shaped satellite (principal moment
of inertia: A < B < C, is the orientation relative to the direction of periapse of the orbit, f = f(t) is the true anomaly, and r = r(t) is the distance from the planet), equation of motion (e.o.m):
C
ABf
r
GM
2
)(3 ;2cos
3
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Spin-orbit Resonance (2)
Rotational symmetry (B = C): no torque from the planet and the satellite’s spin in unperturbed
If B C and the orbit is circular, e.o.m is similar to that of the common pendulum
The width of the 1:1 spin-orbit resonance (n is the orbital mean motion) is
n 22Δ
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Spin-orbit Resonance (3)
Case when the orbit is non-circular and small eccentricity
2212 2sin72sin2sin entntentn
Two new terms corresponding to the 1:2 and the 3:2 spin-orbit resonances
The width of the 3:2 spin-orbit resonance is a factor (7e/2) smaller than the 1:1
Ex.: the 3:2 spin orbit resonance of Mercury (88d:59d)
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Orbital Resonances (1)
Three degrees of freedom: three angular variables [1] the motion of the planet: the frequency revolution
around the Sun,
[2] orientation of the orbit in space: the slow frequencies of precession of the direction of perihelion and the pole of the orbit plane
For a multi-planet system: secular resonances involves commensurabilities amongst [2]; mean motion resonances are commensurabilities of [1]
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Orbital Resonances (2) Most cases: a clear separation of [1] & [2] time
scales A coupling between [1] & [2] chaotic dynamics The boundaries (or separatrices) of mean
resonances are often the site for such interactions between secular and mean motion resonances
Ex. of “hybrid” resonance (a commensurability of a secular precession frequency with an orbital mean motion): the angular velocity of the apsidal precession rate of a ringlet within the C-ring of Saturn is commensurate with the orbital mean motion of Titan the Titan 1:0 apsidal resonance
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Mean Motion Resonance (MMR)
First order resonance
Second order resonance
21
32
~/Δ enn
21
2 ~/Δ enn
Malhotra 1998
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MMR (2)
o Mean motion commensurabilities amongst the Jovian and Saturnian satellites
o No exact resonance in the Uranian satellites system
o The role of the small but significant splitting of MMR and the interaction of neighboring resonances
o Destabilize a previously established resonance MMR lifetimes
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MMR (3): Stability
Stable
Unstable
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Nesvorný et al. 2002
MMR (4): chaotic diffusion
2J:1 & 3J:1 MMR
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MMR (5): MBAs global structure• Overlapping MMR causes chaotic orbits• “Stable chaos”: have strongly chaotic orbits yet are
stable on long interval time (three-body resonances)
Nesvorný et al. 2002
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MMR (6): MBAs global structure
Each resonance corresponds to one V-shaped region except the large first-order MMRs with Jupiter
Nesvorný et al. 2002
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Secular Resonances (1)
• A planetary precessing ellipse of fixed semimajor axis, ap, eccentricity, ep, and precession rate pp g
• g0 is proportional to the mass of the perturbing planet and is also a function of the orbital semimajor axis of the particle relative to that of the planet
• Secular resonance occurs when g0 equals gp
• Effect: to amplify the orbital eccentricity of the particle
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Secular Resonances (2)
Specific secular resonance: “Kozai resonance”, or “Kozai mechanism”
1:1 commensurability of the secular precession rates of the perihelion and the orbit normal such that the argument of perihelion is stationary (or librates)
Requires significant orbital eccentricity and inclination (causes coupled oscillations)
Well known ex.: Pluto whose argument of perihelion librates about 90 deg.
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Secular Resonances (3)
Empty zones along resonant surfaces
Isolation of groups (Hungaria, Phocaea)
Carruba & Michtchenko 2007
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New Result (Carruba & Michtchenko 2007)
Identifying families: Frequency approach
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New Result (Carruba & Michtchenko 2007)
Eos
Koronis