Astronomical Observational Techniques and Instrumentation Professor Don Figer
Astronomical Observational Techniques and Instrumentation Professor Don Figer Energy sources of astronomical objects 1
Aims and outline for this lecture • describe energy sources of astronomical objects – – stars: nuclear reactions protostars: gravitational energy nebulae/clouds: stellar heating and ionizing radiation galaxy clusters: shocks • give case studies of using multiwavelength data to analyze two star clusters 2
Stellar Structure 3
Solar Atomic Abundances 4
Solar System Atomic Abundances 5
Stars: energy source: proton-proton chain 6
Stars: energy source: proton-proton chain PPI (85% for Sun): H 1 + H 1 -> D 2 + e+ + nu(1) (1. 442 Me. V) D 2 + H 1 -> He 3 + gamma (5. 493 Me. V) He 3 + He 3 -> He 4 + 2 H 1 (12. 859 Me. V) PPII (15%): H 1 + H 1 -> D 2 + e+ + nu(1) (1. 442 Me. V) D 2 + H 1 -> He 3 + gamma (5. 493 Me. V) He 3 + He 4 -> Be 7 + gamma (1. 586 Me. V) Be 7 + e- -> Li 7 + nu(2) (0. 861 Me. V) Li 7 + H 1 -> He 4 + He 4 (17. 347 Me. V) PPIII (0. 01%): H 1 + H 1 -> D 2 + e+ + nu(1) (1. 442 Me. V) D 2 + H 1 -> He 3 + gamma (5. 493 Me. V) He 3 + He 4 -> Be 7 + gamma (1. 586 Me. V) Be 7 + H 1 -> B 8 + gamma (0. 135 Me. V) B 8 -> Be 8 + e+ + nu(3) (followed by spontaneous decay. . . ) Be 8 -> 2 He 4 (18. 074 Me. V) 7
Stars: energy source: pp chain: Gamow Peak • Protons in center of star – have high energies – have the same charge (they repel each other) • At sufficiently high energy, particles will fuse. 8
Stars: energy source: pp chain timescales 9
Stars: energy source: CNO cycle 10
Stars: energy source: CNO cycle 12 C + 1 H 13 N → 13 N +γ +1. 95 Me. V → 13 C + e+ + νe +2. 22 Me. V 13 C + 1 H → 14 N +γ +7. 54 Me. V 14 N + 1 H → 15 O +γ +7. 35 Me. V → 15 N + e+ + νe +2. 75 Me. V → 12 C + 4 He +4. 96 Me. V 15 O 15 N + 1 H 11
Stars: energy source: CNO cycle • The CNO cycle has several branches that are favored based on temperature. 12
Stars: energy source: CNO vs PP • The CNO cycle produces more energy than the PP chain at higher temperatures. 13
Betelguese and Rigel in Orion Betelgeuse: 3, 500 K (a red supergiant) Rigel: 11, 000 K (a blue supergiant) 14
Blackbody curves for hot and cool stars 15
Two stars • Hotter Star emits MUCH more light per unit area much brighter at short wavelengths. 16
Stars: energy source: Protostars 17
Stars: energy source: Gravitational Energy • As molecular cloud contracts, gravitational potential energy of particles is converted into kinetic energy. • With higher kinetic energies, the collision rate between particles increases, i. e. temperature and thermal radiation increase. • At sufficiently high density, the gas becomes opaque to escaping radiation at shorter wavelengths, making it difficult to observe the star formation process. • The radiation generated by gravitational energy cannot counterbalance the force of gravity of the overlying material. • Temperature increase until nuclear fusion turns on. 18
Star Formation: Hayashi Track hydrostatic equilibrium gravitational energy nuclear fusion 100, 000 years from 4 to 6 10 million years from 6 to 7 timescales depend heavily on mass 19
Stages of Star Formation on the H-R Diagram 20
Arrival on the Main Sequence • The mass of the protostar determines: – how long the protostar phase will last – where the new-born star will land on the MS – i. e. , what spectral type the star will have while on the main sequence 21
Protostar Luminosity Derivation 22
Star Formation: Gravitational Energy: B 68 Optical 1. 2 mm Dust Continuum Near-Infrared C 18 O B 68 is thought to be in hydrostatic equilibrium, such that the outward pressure balances the inward force of gravity. The cloud should contract as it cools/radiates gravitational energy converted into kinetic energy. N 2 H + 23
Disks & infrared emission 102 RY Tau x 10 n. Fn (10 -12 W m-2) 104 1 Vega DL Tau x 2 10 -2 9700 K 1 10 -4 GM Aur / 20 10 -2 0. 1 1 10 1000 Wavelength ( m) b Pic x 0. 1 1 10 1000 Wavelength ( m) Beckwith & Sargent 1996, Nature, 383, 139 -144. 24
Spectrum of Protoostar 25 Mc. Caughrean et al. 1996
Circumstellar Dust Vega Disk Detection l ( m) Flux* Contrast ( Jy) Star/Disk 11 m 2. 4 1. 5 x 107 22 m 400 2 x 104 33 m 1300 3 x 103 Reflected & emitted light detected with a simple coronograph. *per Airy disk 26
Star Formation: Debris Disks BD+31643 27
Dust Clouds: energy source • Dust clouds usually emit radiation that they absorb from stars (internal or external). • Young stars are often the internal heat source for star forming dust clouds, e. g. Sgr B 2, W 49, W 51. 28
Dust Clouds: energy source: Sgr B 2 29
Dust Clouds: energy source: Sgr B 2 30
Dust Clouds: energy source 31
HCHII Regions in Sgr B 2 Gaume et al. 1995 • There are ~100 HCHII regions in Sgr B 2. 32
HCHII Regions in Sgr B 2 De Pree et al. 1998 • The clumps break up into even smaller clumps with sizes ~100 AU and densities >107 cm-3. • Each clump contains an OB star. 33
Dust Clouds: energy source: external heating • • • M 0. 20 -0. 033 molecular cloud is warm (molecular emission in contours) Notice that its surface is ionized (free-free emission in greyscale). Pistol nebula is also ionized and heated. 34
Dust Clouds: energy source: external heating • • • M 0. 20 -0. 033 is externally heated by nearby Quintuplet cluster of massive stars. Notice that its surface is ionized by the nearby hot stars. Pistol is ejecta that is ionized/heated by Pistol star. 35
Dust Clouds: energy source: external heating: Pa-a 36
Nebulae: energy source: stars • The Pistol nebula is heated by the Pistol star that resides at its center. • Note in the figure that the dust thermal emission peaks in the mid -infrared, indicating temperature of a few 100 K. • The starlight fades in relative intensity at longer wavelengths. • Ionized gas emission suggest an external energy source (other hot stars in Quintuplet). 3 um 17 um 37
Galaxy Clusters: energy source: Shock Heating http: //www-astro. physics. ox. ac. uk/~garret/teaching/lecture 2. pdf 38
Galaxy Clusters: energy source: Shock Heating • Over last 10 Billion years there have been many galaxy collisions in galaxy clusters. • When two galaxies pass through each other stars will continue on their original path – more or less. • Interstellar gas clouds collide and cannot pass through each other. • They get stripped and pass into the gravitational well of the cluster. • This fills with very hot shocked gas over time. • So hot it emits x-rays. • Shows matter distribution. (Mostly dark matter again. ) 39
Galaxy Clusters: energy source: Shock Heating blue=x-ray 40
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Multiwavelength View of Energy Sources red=8 um green=6 cm blue=20 cm red=8 um green=5. 8 um blue=3. 6 um 42
Multi-wavelength analysis of star clusters: the cases of GLIMPSE 9 and Cl 1813 -178 GLIMPSE 9 90 cm 43
Cl 1813 -175: Multiwavelength Image Messineo et al. SNR G 12. 82 -0. 02 (2008) Ap. JL, 683, 155� SNR G 12. 72 -0. 0 HESS J 1813 -178 W 33 2 MASS 3. 6 um 8 um 90 cm 44
Cl 1813 -175: Multiwavelength Plot 74 Chandra point sources from Helfand et al. (2007) 45
Cl 1813 -175: NIR Spectroscopy Red supergiant Blue supergiants Keck/NIRSPEC high– and low–resolution spectroscopy 46
Cl 1813 -175: CMD • • 4. 7 kpc 6 -8 Myr Ak=0. 8 mag 2000 -6000 Msun Chandra data from Helfand et al. (2006) 47
Cl 1813 -175: distance • From the radial velocity of star #1, we derive a kinematic heliocentric distance of 4. 7± 0. 4 kpc by using the rotation curve of Brand & Blitz (1993). • We conclude from the CMDs and distance estimates, that the RSG, the WR star, and the BSGs are all part of the same stellar cluster. The average spectrophotometric distance of 3. 7 ± 1. 7 kpc is consistent with the kinematic distance 4. 7± 0. 4 kpc within uncertainties. We assume the kinematic distance. 48
Cl 1813 -175: age and mass • We assume coevality of the evolved objects – 1 WR, 1 RSG, 2 BSGs, and several X–ray emitters. • We conclude that the cluster is 6 − 8 Myr old since this age allows for the coexistence of both WR and RSG stars. • Assuming that the other eight X–ray emitters associated with the cluster, other than the WR star, are BSGs with masses larger than 20 Msun, and by assuming a Salpeter IMF down to 1. 0 Msun, we derive a total initial cluster mass of 2000 Msun. Messineo et al. (2008, Ap. J 683 -155) 49
24 additional massive stars in CL 11813 -178 (Messineo et al. ) 50
GLIMPSE 9: location (l, b)=(22. 76°, -0. 40°) • HST/NICMOS • f. o. v. = 51. 5”x 51. 5”; pixel scale = 0. 2”; filters = F 160 W, F 222 M • exptime = 19. 94 s, 55. 94 s 51
Age = 6 -30 Myr (presence of RSGs) Ak = 1. 6 ± 0. 3 mag #3 4. 2 kpc #4 4. 7 kpc 52
Cluster surroundings Blue = 3. 6 um Green = 90 cm Red = 24 um Giant Molecular cloud – from CO 10^6 Msun -- 4 SNR remnants 53
REG 1 REG 3 REG 4 REG 6 Ongoing ESO observations with SINFONI to observe the brightest stars of REG 1, REG 3, REG 4 and REG 6 54
GLIMPSE 9 and CL 1813 -178 Summary • GLIMPSE 9 and CL 1813 -178 are two young clusters. • The combination of radio and infrared data allowed us to detect their parental clouds, which appear rich in HII regions and SNRs. • With similar studies of other clusters and giant HII regions we will be able to shed light on the initial masses of the supernova progenitors, and therefore on the fate of massive stars. 55
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