Presentation is loading. Please wait.

Presentation is loading. Please wait.

FSU Harry Kroto 2004.

Published byAmber Fitzgerald Modified over 5 years ago

Similar presentations

Presentation on theme: "FSU Harry Kroto 2004."— Presentation transcript:

1 FSU Harry Kroto 2004

2 BIG U Harry Kroto 2004

3 The Universe is BIG Useful Numbers Harry Kroto 2004

4 Survey of the Universe Harry Kroto 2004

5 The Structure of the Universe – dimensions ly
108 1010 108 Clusters of Galaxies 102 – 103 Galaxies in a cluster 1011 Stars in a Galaxy on average 1022 Stars in total 50% Stars 50% Interstellar Matter Harry Kroto 2004

6 Stellar Cycles Harry Kroto 2004

7 Milky Way Fog

8 We can only see about 1/6 (ca 6000ly) of the way to the Galctic Centre due to scattering by gas and dust in the disk

9 21 cm Line Harry Kroto 2004

10 Milky Way Spiral Structure
Harry Kroto 2004

11 G Stellar Collapse Harry Kroto 2004

12 Localised gravitational condensations
Harry Kroto 2004

13 Stellar Synthesis Harry Kroto 2004

14 Hans Bethe

15 Radioastronomy - History
Harry Kroto 2004

16 at: www.nasaimages.org/luna/servlet/detail/nasaNA...

17 at: www.nasaimages.org/luna/servlet/detail/nasaNA...

18 Spectra Interstellar Molecules
Harry Kroto 2004

19 Interstellar Molecules Tables
Gas phase interstellar and circumstellar molecules 2 Atoms 3 Atoms 4 Atoms 5 Atoms 7 Atoms H2 C2H C2H2 C4H C6H C2 CH2 l-C3H C3H2 HC5N CH HCN c-C3H H2CCC CH2CHCN CH+ HNC NH3 HCOOH CH3C2H CN HCO HNCO CH2CO CH3CHO CO HCO+ HOCO+ HC3N CH3NH2 CS HOC+ HCNH+ CH2CN c-CH2OCH2 OH N2H+ HNCS NH2CN 8 Atoms NH NH2 C3N CH2NH CH3COOH NO H2O C3O CH4 HCOOCH3 NS HCS+ H2CS SiH4 a C7H a SiC a H2S C3S C4Si a H2C6 SiO OCS HCCN C5 a HC6H a SiS N2O H3O+ HCCNC CH3C3N SiN a SO2 H2CN HNCCC 9 Atoms SO SiC2 a H2CO H2COH+ CH3C4H HC1 C2S c-SiC3 6 Atoms CH3OCH3 CP a C2O C2H4 a CH3CH2CN SO+ C3 a H2CCCC CH3CH2OH NaC1 a MgNC a CH3OH HC7N A1C1 a MgCN a CH3CN C8H KC1 a NaCN a CH3NC "e 10 Atoms A1F a HNO CH3SH CH3C4CN ? PN H3+ NH2CHO CH3COCH3 CO+ HC3HO HC9N SiH ? C5H HC11N HF ? HC3NH+ (C2H5)2O ? C5N HC4H a Interstellar Molecules Tables Harry Kroto 2004

20 HOCO+ Harry Kroto 2004

21 Interstellar Clouds Summary
Harry Kroto 2004

22 Red Giant Spectra Harry Kroto 2004

23 Harry Kroto 2004

24 Orion Harry Kroto 2004

25 Orion Japanese Site

26 Weighing Orion Harry Kroto 2004

27

28

Download ppt "FSU Harry Kroto 2004."

Similar presentations

School of Chemistry, University of Nottingham,UK 1 Why Does Star Formation Need Surface Science? Using Laboratory Surface Science to Understand the Astronomical.

School of Chemistry, University of Nottingham,UK 1 Why Does Star Formation Need Surface Science? Using Laboratory Surface Science to Understand the Astronomical.
Radio Waves Where do they come from?. Radio waves belong to a family The electromagnetic spectrum (EM) is a continuum of waves, sometimes called electromagnetic.

Radio Waves Where do they come from?. Radio waves belong to a family The electromagnetic spectrum (EM) is a continuum of waves, sometimes called electromagnetic.
Considerations for Millimeter-wave Observations Amy Lovell, Agnes Scott College Fifth NAIC/NRAO Single-Dish Summer School July 2009.

Considerations for Millimeter-wave Observations Amy Lovell, Agnes Scott College Fifth NAIC/NRAO Single-Dish Summer School July 2009.
The Evolution of Matter: From Simple to Complex Prof. Jackson CC105.

The Evolution of Matter: From Simple to Complex Prof. Jackson CC105.
Chapter 11: The Interstellar Medium Region in the Constellation Orion named the Orion Nebula which is the closest star formation region to us. Jets and.

Chapter 11: The Interstellar Medium Region in the Constellation Orion named the Orion Nebula which is the closest star formation region to us. Jets and.
Star Formation in our Galaxy Dr Andrew Walsh (James Cook University, Australia) Lecture 2 – Chemistry and Star Formation 1.Basic chemical interactions.

Star Formation in our Galaxy Dr Andrew Walsh (James Cook University, Australia) Lecture 2 – Chemistry and Star Formation 1.Basic chemical interactions.
Laboratory Studies of Organic Chemistry in Space A. Ciaravella Palermo, 2014 March 26  InterStellar Medium (ISM) overview  ISM composition  Dust and.

Laboratory Studies of Organic Chemistry in Space A. Ciaravella Palermo, 2014 March 26  InterStellar Medium (ISM) overview  ISM composition  Dust and.
Spectral Line Survey with SKA Satoshi Yamamoto and Nami Sakai Department of Physics, The Univ. of Tokyo Tomoya Hirota National Astronomical Observatory.

Spectral Line Survey with SKA Satoshi Yamamoto and Nami Sakai Department of Physics, The Univ. of Tokyo Tomoya Hirota National Astronomical Observatory.
The Chemistry in Interstellar Clouds Eric Herbst Departments of Physics, Astronomy, and Chemistry The Ohio State University.

The Chemistry in Interstellar Clouds Eric Herbst Departments of Physics, Astronomy, and Chemistry The Ohio State University.
Outflows and Jets: Theory and Observations Winter term 2006/2007 Henrik Beuther & Christian Fendt 20.10 Introduction & Overview (H.B. & C.F.) 27.10 Definitions,

Outflows and Jets: Theory and Observations Winter term 2006/2007 Henrik Beuther & Christian Fendt Introduction & Overview (H.B. & C.F.) Definitions,
Photoelectron Spectrometers Survey of the Universe Harry Kroto 2004.

Photoelectron Spectrometers Survey of the Universe Harry Kroto 2004.
John E. Hibbard North American ALMA Science Center (NAASC/NRAO) Josh Barnes Institute for Astronomy U. Hawai’i (simulating the dynamics of the…) Gas in.

John E. Hibbard North American ALMA Science Center (NAASC/NRAO) Josh Barnes Institute for Astronomy U. Hawai’i (simulating the dynamics of the…) Gas in.
Molecular Survival in Planetary Nebulae: Seeding the Chemistry of Diffuse Clouds? Jessica L. Dodd Lindsay Zack Nick Woolf Emily Tenenbaum Lucy M. Ziurys.

Molecular Survival in Planetary Nebulae: Seeding the Chemistry of Diffuse Clouds? Jessica L. Dodd Lindsay Zack Nick Woolf Emily Tenenbaum Lucy M. Ziurys.
A Study of HCO + and CS in Planetary Nebulae Jessica L. Edwards Lucy M. Ziurys Nick J. Woolf The University of Arizona Departments of Chemistry and Astronomy.

A Study of HCO + and CS in Planetary Nebulae Jessica L. Edwards Lucy M. Ziurys Nick J. Woolf The University of Arizona Departments of Chemistry and Astronomy.
In fact all our atoms were formed in a star long ago.

In fact all our atoms were formed in a star long ago.
Interstellar Chemical Models with Molecular Anions Eric Herbst, OSU T. Millar, M. Cordiner, C. Walsh Queen’s Univ. Belfast R. Ni Chiumin, U. Manchester.

Interstellar Chemical Models with Molecular Anions Eric Herbst, OSU T. Millar, M. Cordiner, C. Walsh Queen’s Univ. Belfast R. Ni Chiumin, U. Manchester.
The ALMA view of a Carbon Rich AGB Star: The Spectrum of IRC+10216

The ALMA view of a Carbon Rich AGB Star: The Spectrum of IRC+10216
365 x 24 x 60 x 60 Harry Kroto 2004 365 x 24 x 60 x 60 = 0.36 x 2.4 x 0.36 x 10 2 x 10 x 10 4 Harry Kroto 2004.

365 x 24 x 60 x 60 Harry Kroto x 24 x 60 x 60 = 0.36 x 2.4 x 0.36 x 10 2 x 10 x 10 4 Harry Kroto 2004.
ASTR112 The Galaxy Lecture 9 Prof. John Hearnshaw 12. The interstellar medium: gas 12.3 H I clouds (and IS absorption lines) 12.4 Dense molecular clouds.

ASTR112 The Galaxy Lecture 9 Prof. John Hearnshaw 12. The interstellar medium: gas 12.3 H I clouds (and IS absorption lines) 12.4 Dense molecular clouds.
Chapter 14 The Interstellar Medium. All of the material other than stars, planets, and degenerate objects Composed of gas and dust ~1% of the mass of.

Chapter 14 The Interstellar Medium. All of the material other than stars, planets, and degenerate objects Composed of gas and dust ~1% of the mass of.

Similar presentations

Ads by Google