The Milky Way Dr Bryce 29:50Slide 2
Class sees Homework: We are moving towards the end of semester, it is imperative that you augment your evaluation by finishing all your homework CSP watching activity Exam conductSlide 3
The Milky Way world shows up in our sky as a weak band of lightSlide 4
âAll sky viewâ The Milky Way in Visible lightSlide 5
Dusty gas mists darken our perspective in light of the fact that they ingest noticeable light This is the interstellar medium that makes new star frameworksSlide 6
Interstellar Medium Can both ingest and transmit light Most of the interstellar medium is gas and it is simplest to watch when it shapes a discharge cloud/cloud Good cases of this incorporate the Orion Nebula Because the gas is prevalently hydrogen we see lines connected with nuclear or ionized hydrogenSlide 7
We see our universe edge-on Primary elements: circle, swell, corona, globular groupsSlide 8
Globular bunches We know from our H-R charts that globular bunches are old One approach to delineate Milky Way is to consider the conveyance of globular groupsSlide 9
Mapping Globular bunchesSlide 10
If we could see the Milky Way from over the plate, we would see its winding armsSlide 11
Our understanding of the Milky Way Disk is slight and wide Note winding arms and barSlide 12
Stars in the plate all circle in the same course with a little all over movementSlide 13
Orbits of stars in the lump and radiance have irregular introductionsSlide 15
Sunâs orbital movement (sweep and speed) lets us know mass inside Sunâs circle: 1.0 x 10 11 M Sun speaks the truth 8kpc from the galactic focusSlide 16
Orbital Velocity Law The orbital pace ( v ) and separation from the galactic focus ( d ) of an article on a roundabout circle around the cosmic system lets us know the mass ( M ) inside of that circleSlide 17
Star-gas-star cycle Recycles gas from old stars into new star frameworksSlide 18
High-mass stars have solid stellar winds that blow rises of hot gasSlide 19
HII locales âH twoâ Strong emanation lines A focal hot star discharges UV photons which ionize the hydrogen When an electron is recovered by a proton the HII line is transmittedSlide 20
HII areas Require a hot star to have shaped in a sub-atomic cloud The more sweltering the star the bigger the HII district can be HII areas have a tendency to be red â see the Rosette NebulaSlide 21
Lower mass stars return gas to interstellar space through stellar winds and planetary nebulaeSlide 22
X-beams from hot gas in supernova remainders uncover recently made substantial componentsSlide 23
The Milky Way at X-beam Wavelengths X-beam outflow is delivered by hot gas air pockets and X-beam parallelsSlide 24
Supernova leftover cools and starts to discharge unmistakable light as it extends New components made by supernova blend into interstellar mediumSlide 25
Radio emanation in supernova remainders is from particles quickened to close light speed Cosmic beams presumably originate from supernovaeSlide 26
Multiple supernovae make immense hot air pockets that can victory of plate Gas mists cooling in the corona can rain down on circleSlide 27
Atomic hydrogen gas shapes as hot gas cools, permitting electrons to join with protons Molecular mists structure next, after gas cools enough to permit to iotas to consolidate into atomsSlide 28
Molecular mists in Orion Composition: Mostly H 2 About 28% He About 1% CO Many different atomsSlide 29
Gravity structures stars out of the gas in sub-atomic mists, finishing the star-gas-star cycleSlide 30
Radiation from recently shaped stars is dissolving these star-framing mistsSlide 31
Gas reusing Stars make new components by combination Dying stars remove gas and new components, creating hot air pockets (~10 6 K) Hot gas cools, permitting nuclear hydrogen mists to frame (~100-10,000 K) Further cooling licenses particles to shape, making sub-atomic mists (~30 K) Gravity shapes new stars (and planets) in sub-atomic mists Gas CoolsSlide 32
Interstellar gas temperature Molecular mists are thick and at low temperatures (~10K) Interstellar gas is significantly less thick and much hotter (~10,000K) We additionally see exceptionally hot (~1 million K) gas from Supernova stun waves, it is these locales that are in charge of the X-beam bubblesSlide 33
The Milky Way at 21cm wavelength Neutral hydrogen in bound to the plane of the Milky WaySlide 34
21cm line Associated with the least vitality level of Hydrogen Doesnât include the hydrogen molecule communicating with another photon so we can âseeâ this line anyplace in spaceSlide 35
Dark Nebula Associated with interstellar Dust particles obstruct the photons from the stars behind them Dust will re-emanate in the infra-redSlide 36
The advancement of our Model Galileo initially watched that the Milky Way is made of stars and numerous stargazers have attempted to guide it For instance Herschel utilized star tallies, see beneathSlide 37
Early models Were mistaken as they didnât incorporate the impacts of interstellar dust which will diminish starlight (this impact is called eradication) and interstellar blushing It is thus that we really discover it less demanding to concentrate on different systems instead of the world in which we liveSlide 38
We watch star-gas-star cycle working in Milky Wayâs circle utilizing various wavelengths of lightSlide 39
Halo: No ionization nebulae, no blue stars ï no star development Disk: Ionization nebulae, blue stars ï star arrangementSlide 40
Halo Stars: 0.02-0.2% overwhelming components (O, Fe, â¦), just old stars Halo stars framed to begin with, then ceased Disk Stars: 2% substantial components, stars of all ages Disk stars framed later, continued framingSlide 41
Much of star arrangement in plate happens in winding arms Whirlpool GalaxySlide 42
Spiral Structure We can without much of a stretch watch winding arms in different universes yet inside of the Milky Way our perspective is prevented by the impacts of interstellar gas and dustSlide 43
Spiral arms are influxes of star development Gas mists get pressed as they move into winding arms Squeezing of mists triggers star arrangement Young stars stream out of winding armsSlide 44
Stars moderate down in the winding arms Density WavesSlide 45
Our universe likely framed from a titan gas cloudSlide 46
Halo stars framed first as gravity made cloud contractSlide 47
Remaining gas subsided into turning circleSlide 48
Stars constantly frame in plate as cosmic system becomes more establishedSlide 49
Collisions cause the circle\'s smoothing Upwards or downwards movements have a tendency to be counteracted Cloud crashesSlide 50
Rotation Possible models for revolution Wheel or Merry-go-round Planetary or Keplerian Milky Way doesnât pivot like both of these modelsSlide 51
Milky Wayâs pivot Curve Is âflatâ This implies that the circulation of mass in the Milky Way proceeds outwards past the brilliant material (stars) The dim matter could be cocoa smaller people, white diminutive people, Jupiters, Black openings or basic particles, they are not transmitting light but rather they are applying gravitational impactSlide 52
The obvious bit of a system lies somewhere down in the heart of a huge corona of dull matterSlide 53
We can quantify revolution bends of other winding universes utilizing the Doppler movement of the 21-cm line of nuclear HSlide 54
Spiral systems every one of the tend to have level revolution bends demonstrating a lot of dim matterSlide 55
Gravitational microlensing A dim item in the galactic radiance (MACHO) could go about as a lens as a result of the ebb and flow of spacetime around it. Dark gaps would be the most grounded sort of microlensSlide 56
Infrared light from focus Radio discharge from focusSlide 57
Swirling gas close focus Orbiting star close focusSlide 58
Stars give off an impression of being circling something enormous however imperceptible â¦ a dark gap? Circles of stars demonstrate a mass of around 4 million M SunSlide 59
X-beam flares from galactic focus propose that tidal powers of suspected dark gap every so often tear separated p
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