astronomija kratka povijest problematike. područje interesa planeti sunčev sustav zvijezde ...
TRANSCRIPT
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AstronomijaAstronomijakratka povijest problematikekratka povijest problematike
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Područje interesaPodručje interesa
PlanetPlanetii SSunčev sustavunčev sustav ZvijezdeZvijezde Međuzvjezdani prostorMeđuzvjezdani prostor GalGalaksijeaksije Aktivne galaktičke jezgre (Aktivne galaktičke jezgre (AGNAGN)) Kvazari (eng. quasar - quasi-stellar radio source) Kvazari (eng. quasar - quasi-stellar radio source) Klasteri galaksijaKlasteri galaksija Pulsari (brzorotirajuće neutronske zvijezde)Pulsari (brzorotirajuće neutronske zvijezde) SvemirSvemir
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Sunčev sustavSunčev sustav
Fizika Fizika SSuncaunca SolaSolarni vjetarrni vjetar PlanetPlaneti i Njihovi satelitiNjihovi sateliti AsteroidAsteroidii NEOsNEOs (eng. Near (eng. Near
eart objects)eart objects) PojasiPojasi InterplanetInterplanetarna arna
prašinaprašina
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ZvijezdeZvijezde
promjenjive zvijezdepromjenjive zvijezde dvojne zvijezdedvojne zvijezde patuljci, divovipatuljci, divovi SupernoveSupernove kompaktni objektikompaktni objekti
((crne rupecrne rupe, , bijeli bijeli patuljcipatuljci, neutro, neutronskenske zvijezdezvijezde))
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Međuzvjezdani prostorMeđuzvjezdani prostor
Nastanak zvijezdaNastanak zvijezdaAstro-kemijaAstro-kemijaStruktura i razvoj Struktura i razvoj
zvijezdazvijezdaNuklearna Nuklearna
astrofizikaastrofizika
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GalaksijeGalaksije
Nastanak i Nastanak i formiranjeformiranje
StruStrukturakturaNaseljenostNaseljenostDDinamikainamika
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AGN (Aktivne galaktičke jezgre) AGN (Aktivne galaktičke jezgre) KvazariKvazari
nastanaknastanakklasifikacijaklasifikacijagorivogorivoevolucijaevolucijagustoćagustoća
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KlasteriKlasteri
Nastanak i Nastanak i razvojrazvoj
StruStrukturakturaTamna tvarTamna tvarGravitacijske Gravitacijske
lećeleće
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SvemirSvemir
Starost i veličinaStarost i veličinaNastanak i razvojNastanak i razvojTamna materija , Tamna materija ,
stringovi, egzotične stringovi, egzotične česticečestice
TopoloTopologijagija ( (oblikoblik))
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Znanstveni elementi u astronomijiZnanstveni elementi u astronomiji PromatranjePromatranje
• Zemaljsko Zemaljsko (opti(optičkočko, , infrainfracrvenocrveno, radio), radio)
• VanplanetarnoVanplanetarno ((sateliti i satelitske sateliti i satelitske platformeplatforme; UV, x-ray); UV, x-ray)
RačunanjeRačunanje• AnalAnaliza podatakaiza podataka• KKompleompleksniksni problem problemii• NumeriNumeričke čke simula simulacijecije
AnalAnalizaiza• objeobjektivnostktivnost• asimilasimiliranjeiranje formi i formi i
podatakapodataka• linearlinearnono & & nenelinearlinearnono
razmišljanjerazmišljanje
PisanjePisanje• publikacijapublikacija• prprijedlogaijedloga• preprezentacijazentacija
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ZapošljavanjeZapošljavanje (danas) (danas)
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Što astronomi Što astronomi nene rade rade
Pišu horoskopePišu horoskope Imaju vezu s vanzemaljskim Imaju vezu s vanzemaljskim
civilizacijamacivilizacijama Memoriraju konstelacijeMemoriraju konstelacije Cijelo vrijeme gledaju kroz teleskopCijelo vrijeme gledaju kroz teleskop
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RadioastronomijaRadioastronomija
Kozmičko zračenje 3KKozmičko zračenje 3K
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Elektromagnetski valoviElektromagnetski valovi
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E=hE=h c= c=
Duži valoviNiža energijaNiža frekvencija
Kraćo valoviVeća energijaViša frekvencija
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Elektromagnetski Elektromagnetski spektarspektar
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Elektromagnetski prozor kroz Elektromagnetski prozor kroz atmosferu!atmosferu!
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Izvori elektromagnetskog zračenjaIzvori elektromagnetskog zračenja
TermalniTermalni• Zračenje crnog Zračenje crnog
tijelatijela• Kontinuirana Kontinuirana
emisija ioniziranog emisija ioniziranog plina (plazma)plina (plazma)
• Emisija spektralnog Emisija spektralnog zračenja atoma i zračenja atoma i molekulamolekula
NetermalniNetermalni• Sinkrotronsko Sinkrotronsko
zračenjezračenje• MASERSMASERS
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Plankov zakonPlankov zakonu(ν,T) = 4I(ν,T) / c
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Zračenje crnog tijela - SjajZračenje crnog tijela - Sjaj
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Sjaj elektromagnetskog zračenja različitih valnih dužina za Sjaj elektromagnetskog zračenja različitih valnih dužina za crno tijelo na različitim temperaturamacrno tijelo na različitim temperaturama
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MASERMASER
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Sinkrotronsko zračenjeSinkrotronsko zračenje
PolarizaPolarizacojska svojstvacojska svojstva EM zračenja daju EM zračenja daju informacije o geometriji magnetskog poljainformacije o geometriji magnetskog polja
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Sinkrotronsko zračenjeSinkrotronsko zračenje
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Zakon obrnutog kvadrata !Zakon obrnutog kvadrata !
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ZabludaZabluda
Radio program koji se ne sluša!
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Radio Radio TeleskopiTeleskopi
Dvije izvedbeDvije izvedbe::
Polje radio antena
Green Bank Telescope, WV Very Large Array, NM
Radio antena
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1980 1980 godinegodine Dvadest sedamDvadest sedam
25-m25-metarskih etarskih rekonfigurabilnihrekonfigurabilnihantenantena;a; Socorro, Socorro, NM NM
Više publikacija Više publikacija od bilo kojeg od bilo kojeg teleskopa na teleskopa na svijetusvijetu
The Very Large ArrayThe Very Large Array (VLA) (VLA)
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Very Long Baseline ArrayVery Long Baseline Array (VLBA) (VLBA)
1993 1993 godinegodine OOperirane ozperirane oz
SocorroSocorro-a-a DesetDeset 25-m 25-m
antennas antennas diljemdiljem SADSAD, , KKanadanadee, P.R., P.R.
Najviša Najviša rezolucijarezolucija
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PočeciPočecieksperiment Janskogeksperiment Janskog
Promatra nemodulirani doprinos RF (static)
Postepeno s mijenja intenzitet s periodom od gotovo 24hSunce izvor?maksimum 4 minute rani svaki danIzvor izvan Sunčeva sustavaIzvor u Mlječnoj stazi!1933 objavljuje rezultate
Karl G. Jansky (1905-1950)
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Reberov tip radioteleskopaReberov tip radioteleskopaDespite the implications of Jansky’s work, both on the design of radio receivers, as well as for radio astronomy, no one paid much attention at first. Then, in 1937, Grote Reber, another radio engineer, picked up on Jansky’s discoveries and built the prototype for the modern radio telescope in his back yard in Wheaton, Illinois.
He started out looking for radiation at shorter wavelengths, thinking these wavelengths would be stronger and easier to detect. He didn’t have much luck, however, and ended up modifying his antenna to detect radiation at a wavelength of 1.87 meters (about the height of a human), where he found strong emissions along the plane of the Milky Way.
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Reconfigurable Arrays: Zoom Lens Effect Reconfigurable Arrays: Zoom Lens Effect
Više Više detektora – detektora – bolja bolja rezolucijarezolucija
VLAVLBA
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Radio Telescopes: SensitivityRadio Telescopes: Sensitivity
• VLA B-array: Total VLA B-array: Total telescope telescope collecting area is collecting area is only 0.02% of land only 0.02% of land areaarea
More spread-out More spread-out arrays can only arrays can only image very image very bright, compact bright, compact sourcessources
• Sensitivity (how faint of a thing you can “see”) depends on how much of the area of the telescope/array is actually collecting data
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Green Bank Telescope, WV
Parabolic DishParabolic Dish
Aluminum Aluminum reflecting reflecting surface surface
Focuses Focuses incoming waves incoming waves to prime focus to prime focus or sub-reflectoror sub-reflector
Sub-reflector
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Sub-reflectorSub-reflector
Feed Pedestal
Sub-reflector
• Re-directs incoming waves to Feed Pedestal
• Can be rotated to redirect radiation to a number of different receivers
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1.5GHz 20cm 2.3GHz 13cm 4.8GHz 6cm 8.4GHz 4cm 14GHz 2cm 23GHz 1.3cm 43GHz 7mm 86GHz 3mm
327MHz 90cm610MHz 50cm
Feed PedestalFeed Pedestal
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Antenna Feed and Antenna Feed and ReceiversReceivers
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Benefits of Observing in the Benefits of Observing in the RadioRadio
Track physical processes with no Track physical processes with no signature at other wavelengthssignature at other wavelengths
Radio waves can travel through dusty Radio waves can travel through dusty regions regions
Can provide information on magnetic Can provide information on magnetic field strength and orientationfield strength and orientation
Can provide information on line-of-sight Can provide information on line-of-sight velocitiesvelocities
Daytime observing (for cm-scale Daytime observing (for cm-scale wavelengths anyway)wavelengths anyway)
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Primary Astrophysical Processes Primary Astrophysical Processes Emitting Radio RadiationEmitting Radio Radiation
Synchrotron RadiationSynchrotron Radiation• Charged particles moving along magnetic field Charged particles moving along magnetic field
lineslines Thermal emission Thermal emission
• Cool bodiesCool bodies• Charged particles in a plasma moving aroundCharged particles in a plasma moving around
Spectral Line emissionSpectral Line emission• Discrete transitions in atoms and molecules Discrete transitions in atoms and molecules
When charged particles change direction, they emit radiation
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Thermal EmissionThermal Emission
Emission from warm Emission from warm bodiesbodies• ““Blackbody” radiation Blackbody” radiation • Bodies with Bodies with
temperatures of ~ 3-temperatures of ~ 3-30 K emit in the mm 30 K emit in the mm & submm bands& submm bands
Emission from Emission from accelerating accelerating charged particlescharged particles• ““Bremsstrahlung” or Bremsstrahlung” or
free-free emission free-free emission from ionized plasmasfrom ionized plasmas
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Nobelova nagrada za otkriće Nobelova nagrada za otkriće kozmičkog mikrovalnog kozmičkog mikrovalnog pozadinskog zračenjapozadinskog zračenja
Arno Allan Penzias Robert Woodrow Wilson
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The Nobel Prize in Physics 1993The Nobel Prize in Physics 1993
for the discovery of a new type of for the discovery of a new type of pulsar, a discovery that has opened pulsar, a discovery that has opened up new possibilities for the study of up new possibilities for the study of gravitation" gravitation"
Russell A. Hulse Joseph H. Taylor Jr
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Emits photon with a wavelength of 21 cm (frequency of 1.42 GHz)
Spectral Line emission: hyperfine Spectral Line emission: hyperfine transition of neutral Hydrogentransition of neutral Hydrogen
Transition probability=3x10-15 s-1 = once in 11 Myr
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Spectral Line emission: Spectral Line emission: molecular rotational and molecular rotational and
vibrational modesvibrational modes Commonly observed Commonly observed
molecules in space:molecules in space:• Carbon Monoxide (CO)Carbon Monoxide (CO)
• Water (HWater (H22O), OH, HCN, O), OH, HCN, HCOHCO++, CS, CS
• Ammonia (NHAmmonia (NH33), ), Formaldehyde (HFormaldehyde (H22CO)CO)
Less common Less common molecules:molecules:• Sugar, Alcohol, Antifreeze Sugar, Alcohol, Antifreeze
(Ethylene Glycol), …(Ethylene Glycol), …
malondialdyde
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Spectral Line Doppler effectSpectral Line Doppler effect
Spectral lines have fixed Spectral lines have fixed and very well determined and very well determined frequenciesfrequencies
The frequency of a source The frequency of a source will changed when it moves will changed when it moves towards or away from youtowards or away from you
• Comparing observed frequency to known frequency tells you the velocity of the source towards or away from you
Sees original wavelength
Sees shorter wavelength
Sees longer wavelength
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Special example of Spectral Special example of Spectral Line observation:Line observation:Doppler Radar ImagingDoppler Radar Imaging
Transmit radio wave with well defined frequency…
..observe same frequency
…bounce off
object…
NASA’s Goldstone Solar System Radar Very Large Array
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Brief Tour of the Radio UniverseBrief Tour of the Radio Universe
Solar SystemSolar System• Sun, Planets, AsteroidsSun, Planets, Asteroids
Galactic objectsGalactic objects• Dark clouds, proto-stellar disks, supernova Dark clouds, proto-stellar disks, supernova
remnants, remnants, GalaxiesGalaxies
• Magnetic fields, neutral hydrogenMagnetic fields, neutral hydrogen Radio Jets Radio Jets The UniverseThe Universe
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K-band 23 GHz
Ka-band 33 GHzQ-band 41 GHzV-band 61 GHzW-band 94 GHz
Shepherding in the era of “Precision Cosmology”
Background=3 K blackbody radiation
Wilkinson Microwave Anisotropy Probe Wilkinson Microwave Anisotropy Probe (WMAP)(WMAP) map.gsfc.nasa.gov
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image of the image of the cosmic microwave background radiation radiation anisotropy. It has the most precise . It has the most precise thermal emission spectrum known and corresponds to a temperature of 2.725 spectrum known and corresponds to a temperature of 2.725 kelvin (K) (K)
with an emission peak at 160.2 with an emission peak at 160.2 GHz
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Radio pregled Mlječne stazeRadio pregled Mlječne staze
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(a) radio (b) infrared, (c) visible(d) X-rayEach illustration shows the Milky Way stretching horizontally across the picture.
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PulsarPulsar PulsarsPulsars are highly magnetized, rotating are highly magnetized, rotating
neutron stars that emit a beam of that emit a beam of electromagnetic radiation. The observed . The observed periods of their pulses range from 1.4 periods of their pulses range from 1.4 milliseconds to 8.5 seconds. The radiation to 8.5 seconds. The radiation can only be observed when the beam of can only be observed when the beam of emission is pointing towards the emission is pointing towards the Earth. .
This is called the lighthouse effect and gives This is called the lighthouse effect and gives rise to the pulsed nature that gives pulsars rise to the pulsed nature that gives pulsars their name. Because neutron stars are very their name. Because neutron stars are very dense objects, the rotation period and thus dense objects, the rotation period and thus the interval between observed pulses are the interval between observed pulses are very regular. For some pulsars, the regularity very regular. For some pulsars, the regularity of pulsation is as precise as an of pulsation is as precise as an atomic clock..
Pulsars are known to have planets orbiting Pulsars are known to have planets orbiting them, as in the case of them, as in the case of PSR B1257+12. . Werner Becker of the Werner Becker of the Max-Planck-Institut für extraterrestrische Physik said in 2006, "The theory of how pulsars said in 2006, "The theory of how pulsars emit their radiation is still in its infancy, even emit their radiation is still in its infancy, even after nearly forty years of work.after nearly forty years of work.
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KvazarKvazar A A Quasi-stellar radio sourceQuasi-stellar radio source ( (QuasarQuasar) is a powerfully ) is a powerfully
energetic and distant energetic and distant galaxy with an with an active galactic nucleus. Quasars were first identified as being high . Quasars were first identified as being high redshift sources sources of of electromagnetic energy, including , including radio waves and and visible light, that were point-like, similar to , that were point-like, similar to stars, rather , rather than extended sources similar to than extended sources similar to galaxies..
While there was initially some controversy over the nature While there was initially some controversy over the nature of these objects — as recently as the 1980s, there was no of these objects — as recently as the 1980s, there was no clear consensus as to their nature — there is now a clear consensus as to their nature — there is now a scientific consensus that a quasar is a compact region 10- that a quasar is a compact region 10-10,000 10,000 Schwarzschild radii across surrounding the central across surrounding the central supermassive black hole of a galaxy, powered by its of a galaxy, powered by its accretion disc..
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MaserMaser [edit] Historical background[edit] Historical background In 1965 an unexpected discovery was made by Weaver In 1965 an unexpected discovery was made by Weaver et al.et al.[3] - emission lines in [3] - emission lines in
space of unknown origin at a frequency of 1665 MHz. At this time many people still space of unknown origin at a frequency of 1665 MHz. At this time many people still thought that molecules could not exist in space, so the emission was at first put thought that molecules could not exist in space, so the emission was at first put down to an interstellar species named down to an interstellar species named MysteriumMysterium, but the emission was soon , but the emission was soon identified as line emission from OH molecules in compact sources within molecular identified as line emission from OH molecules in compact sources within molecular clouds[4]. More discoveries followed, with H2O emission in 1969[5], CH3OH emission clouds[4]. More discoveries followed, with H2O emission in 1969[5], CH3OH emission in 1970[6] and SiO emission in 1974[7], all coming from within molecular clouds. in 1970[6] and SiO emission in 1974[7], all coming from within molecular clouds. These were termed "masers", as from their narrow line-widths and high effective These were termed "masers", as from their narrow line-widths and high effective temperatures it became clear that these sources were amplifying microwave temperatures it became clear that these sources were amplifying microwave radiation.radiation.
Masers were then discovered around highly evolved Masers were then discovered around highly evolved Late type starsLate type stars; First was OH ; First was OH emission in 1968[8], then H2O emission in 1969[9] and SiO emission in 1974[10]. emission in 1968[8], then H2O emission in 1969[9] and SiO emission in 1974[10]. Masers were also discovered in external galaxies in 1973[11], and in our own solar Masers were also discovered in external galaxies in 1973[11], and in our own solar system in comet halos.system in comet halos.
Another unexpected discovery was made in 1982 with the discovery of emission from Another unexpected discovery was made in 1982 with the discovery of emission from an extra-galactic source with an unrivalled luminosity about 106 times larger than an extra-galactic source with an unrivalled luminosity about 106 times larger than any previous source[12]. This was termed a any previous source[12]. This was termed a megamasermegamaser because of its great because of its great luminosity, and many more megamasers have since been discovered.luminosity, and many more megamasers have since been discovered.
Evidence for an Evidence for an anti-pumpedanti-pumped (dasar) sub-thermal population in the 4830 MHz (dasar) sub-thermal population in the 4830 MHz transition of formaldehyde (H2CO) was observed in 1969 by Palmer transition of formaldehyde (H2CO) was observed in 1969 by Palmer et al.et al.
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