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| (3)minor bodies in solar sys |
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Definition
| dwarf plts, comets, asteroids |
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| orbit sun, have sufficient mass, havent cleared nbhd ar orbit, arent sats. pluto, ceres, charon, xena, quaoar |
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| sim to jup, gassy, lg, massive, low density, far f sun. jup saturn uranus neptune |
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| deted by its orbital eccentricity. Es mass= 1.00 |
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| ratio of amt of matter of obj compared to its V. Es dens= 5.52 |
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| mass (f watching orbits of sats) and V (f m.ing angular sz and d to get r) |
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| orbit in same dir, rot in same dir runt themselves (*alm all), orbit in same plane (wi 10deg of ecliptic), have alm circular orbits |
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| cel body t orbits sun, has sufficient mass, nearly round shape, has cleared nbhd runt its orbit. deted by IAU in 06 |
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| first ast to be disced (1801). was classed as plt |
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| disced 1930 as obj, not plt. has sats (moons), atm at perihelion. mass=.2% Es mass. extremely low density - sig portion must be ice |
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| circular orbit. it and pluto orbit eo. its moon is tidally locked to pluto. mass=10% plutos mass. r= 1/2 plutos r |
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| high eccentric/elliptical. Crosses Neps orbit (as do other kuiper belt objs). Inclined at 17deg. Doesnt orbit in ecliptic plane. Hasnt cleared path of orbit (T, is not plt). |
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1. cloud of dust and gas rotated ltly.
2. contracted under G, spun faster.
3. center blev sun, outer disk blev plts.
Expls sys's flat shape and plts rotn runt sun |
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| m of objs tendency to keep rotating and maintain orientation |
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J= m(mass) * v(rotl v) * r(sz)
J= l(rotl inertia) * w(angular v) |
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| enormous rotating aggregate of cloud and dust. all stars formed f them |
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| a few lt yrs in D, contained ab twice suns mass, comp sim to suns atm today |
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1. G pulling in + outward push f rotn = bulge
2. cloud rotn rate incs due to angular mom
3. partles spd up, incing gas and dust temp
4. partles collide. lose e in dir
perpendicular to clouds rotn
5. disk flattens |
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Definition
1. sm dust grains (interstellar dust) condense into ice/water in outer parts of disk, bc theyre farthest f sun
2. pltesimals form due to accretion
3. inced mass Gly attracts more nebular debris |
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| prob not accretion. formed directly f dense gas regions in disk. G allowed capture and retention of atm |
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| (4)What chars of jovian plts are due to their form.n? |
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Definition
| low temp, dense cores, lots of H, massive atm |
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| (2-7)retention of plts atm due lgly to |
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Definition
| its sz (m and r) and d f sun (T, surf temp -> spd of mols -> esc v?) |
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| (2)gas mols move faster for |
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Definition
| lter mols and jovian plts |
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| inner structure of t plts |
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Definition
| mantle of silicate rock, core of iron/nickel |
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| inner structure of j plts |
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| mantle of gas, core of iron and rock |
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| accretion leaves excess dust. grains smer th .1 um are pushed out sol sys by radn pressure f sun |
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| very sm pressure exerted on partles by sunlt. picture lt as stream of partles (photons) w mom |
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| (5)infl of radn pressure deps on |
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| sz, material, shape, and structure of dust grains, and temp of star (sun) |
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| lt reflected f dust partles. shows us dust in sol sys. we see it shortly after sunset and b4 sunrise |
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| grinding dn of ast.al bodies, evaporation of cometary bodies |
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| tiny partles t condensed f neb stick ihop |
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| Hm sats are there in the sol sys? |
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| nearly circ. in same dir as plt spins. close to plane of plts =tor |
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| scaled-dn version of sol neb |
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| maria (dark As) + terrae (lt As) + craters |
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| phobos (lger, denser, closer) and deimos. irreg shps, craters. syn rot pds. |
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| io europa ganymede callisto (lgest, farthest, lowest dens, most inclined) |
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| aka galilean moons/sats. 63 total. syn rot orbits. |
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| lgest moon in sol sys (lger th mercury). mo rock, water, metallic core. thin o2 atm |
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| one of 61 saturn moons. syn rot orbit. dense n2 atm. liquid h2 lakes. surf is young |
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| 27 known. miranda ariel umbriel. dark. no atm |
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| lgest of 13 nep moons. syn rot pd |
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| nucleus, coma (cloud of dust runt n), tails |
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| core of frozen gases and dust t make up comet's solid part |
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| mo rock dust ice water frozen gases. irreg-shped bodies. dark |
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| objs t orbit sun beyond neps orbit (40 AU) |
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| hyp.ed spherical cloud of comets t surrounds sol sys, beyond plutos orbit (10-100thou AU). Gases and ices still frozen. No confirmation so far |
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| ions. blue. infled by sol wind. dired away f sun. lgest part of comet. sm mass |
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| yellow-white. infled by radn pressure. bent towards comets orbit. wide |
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| orbital pd < 200yrs. orig in kuiper belt. low inclination, close to ecliptic. ex: halley (T=76 yrs, very elliptical orbit) |
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| orbital pd > 200yrs. orig in oort cloud. ex: hale-bopp (T=2533 yrs, alm perfectly elliptical orbit) |
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| E passing thru trail of dust left by comet |
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| Why can you see a comets coma when it comes near the sun? |
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| surf temp incs, comet blir active. ice under surf hts up, hay explosion on surf |
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| (3)hydrostatic equilibrium |
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| G inward + gas pressure outward. P below > P above. Sun will remain same sz as long as it conts prod.ing e at sm rate |
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| e prodn (radiated by nr fusion). has temp 15mil K. plasma at center supports entire mass of sun |
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| e transported by em radn (photons) |
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| e carried by convection. atoms are less completely ionized. e trapped and hts gas |
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| em radn escs -> vis surf. source of absorption sp. low-dens. gas grows denser below and thinner above |
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| lower atm. coolest part, but temp rises as r incs. can be seen as red ln in complete sol eclipse. source of emission sp |
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| rapid inc in temp in these few 100km |
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| upper/outer atm. can be seen in vis lt in total sol eclipse. extremely hot gas w low dens. infled by mag field. |
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| core, radiative zone, convection zone, photosphere, chromosphere, corona |
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| low-dens gases t lie above pho. chr + cor |
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| analysis of pressure waves on sol srf. only way to view sol interior. |
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| n (pns + nns) and ens in orbit ar n |
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| has same # pns but diff # nns |
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| A= mass # (pns + nns), Z= atomic # (pns) |
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| process t binds 2 or more atomic n into one heavier one. E=(delta)m*c^2 |
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| high temp (at least 10^7 K), high dens (so t collisions are common) |
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1. 2 pns (1H n) fuse ihop =>
2H isotope (n of 1 pn+1 nn)
2. 2H n collides w 1H n => 3He isotope
3. 2 3He n fuse => 4He and 2 1H n.
2 pns ejected by elec propulsion |
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| converts H to He, using C as catalyst. occurs in higher-temp stars |
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| Hm mass is converted into e every sec? |
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| seemingly empty region in ast belt. d at wh ast would have orbital pd 1/3 jups |
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| asts t orbit jup in 2 stable pts: 60deg b4 and behind it. |
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| dense mat settles to core of obj, leaving lter mat on srf/mantle. temp must be high enuf t mat can melt |
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| fragments of asts collected on Es srf |
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| sm objs moving in sol sys |
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| pt where sol wind is no longer strong enuf to push back interstellar med. often considered outer boundary of sol sys. d unknown, but lies far outside pluto |
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| d where interstellar wind starts to decelerate into sol wind |
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| ched partles moving away f sun. loses ab 10mil tons mat/yr. confines mag fields. |
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| stellar seq (hot to cold) |
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| O (blue) A (white) G (yellow) M (red) |
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| ch in absorption lns due to |
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| have less H lns bc hay less atomic H. He is dom |
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| are cool enuf to form mols. H lines absent due to lack of excitation e |
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| suns srf and atmic activity |
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1. sun rotates faster at =tor
2. mag field lines wind ar =tor, coils ar sun
3. kinks dev t break thru srf and come back in at sun spots (N and S poles) |
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| What makes the mag field strong? |
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| plasma (ionized gas) and sol rotn |
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| are cool (4500K). bright. very strong mag field. prevents transport of e |
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| sp lns split into sev lns in presence of strong mag field (sun spots). used to m mag field on pho |
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| ionized gas ejected f suns pho following mag field out of srf and back in, along mag loops |
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| 2 spots come ihop, their field lines join. mat t was following field lns explodes away f sun |
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| 22 yrs. every 11 yrs polarity (order of N/S lding/falling spots) is reversed. sm # spots start at high lats, move toward =tor and dec in # |
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| d at wh Es orbit gives a parallax of 1" (arcsec). PARallax in arcSEConds. =3.26 lt yrs |
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| displacement of obj viewed along 2 diff lns of sight. star appears shifted. exists bc E moves in spc |
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| half of total angular 2 bw lns. d(pc)=1/p (arcsec). closer objs have lger par. would be easier to m if E had lger orbit |
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| (3)w ground=based tels, we can m par |
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| >.02 arcsec, d<50 pc. we cant see stars farther away th 500 pc |
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