Trends in the Chandra X-Ray Spectra of O and Early B Stars June 24, 2008.

Slides:

Advertisements

Similar presentations

Unresolved X-Ray Sources in Intermediate Redshift Cluster Fields Unresolved X-Ray Sources in Intermediate Redshift Cluster Fields S. Fawcett, A. Hicks,

Advertisements

Introduction to Astrophysics Ronald L. Westra Department Mathematics Maastricht University.

Deriving direct mass measurements of black holes in ULXs Jeanette Gladstone, T. Roberts, C. Copperwheat, A. Goulding, C. Heinke, A Swinbank, T. Cartwright,

Strange Galactic Supernova Remnants G (the Tornado) & G in X-rays Anant Tanna Physics IV 2007 Supervisor: Prof. Bryan Gaensler.

X-ray Properties of Five Galactic SNRs arXiv: Thomas G. Pannuti et al.

X-ray Diagnostics and Their Relationship to Magnetic Fields David Cohen Swarthmore College.

Tidal Disruptions of Stars by Supermassive Black Holes Suvi Gezari (Caltech) Chris Martin & GALEX Team Bruno Milliard (GALEX) Stephane Basa (SNLS)

X-ray Emission and Absorption in Massive Star Winds Constraints on shock heating and wind mass-loss rates David Cohen Swarthmore College.

X-ray Diagnostics and Their Relationship to Magnetic Fields David Cohen Swarthmore College.

Line Shapes in Hot Stars: Hydrodynamics & Wind Mass-Loss Rates David Cohen Swarthmore College with Maurice Leutenegger, Stan Owocki, Rich Townsend, Emma.

X-ray Diagnostics and Their Relationship to Magnetic Fields David Cohen Swarthmore College.

X-rays from Young Massive Stars David Cohen Swarthmore College.

A pair of O stars with hard X-rays in M17 Marc Gagné & David Cohen Chandra optical.

X Ray Astronomy Presented by:- Mohit Shashwat Ankit.

Wind Signatures in the X-ray Emission Line Profiles of the O Supergiant  Orionis Kevin Grizzard 1, David Cohen 2, Maurice Leutenegger 3, Casey Reed 2,

Spectra of different kinds of celestial objects Makemake.

X-ray Emission Line Profiles of Hot Stars David H. Cohen and Stanley P. Owocki Presented at “Two Years of Chandra Science” Washington, D.C., September.

Wavelength flux Spectral energy distributions of bright stars can be used to derive effective temperatures Ay 123 Lecture I - Physical Properties.

IR Shell Surrounding the Pulsar Wind Nebula G SNRs and PWNe in the Chandra Era Boston, July 8, 2009 Tea Temim (CfA, Univ. of MN) Collaborators:

The Application of Forbidden Line X-Ray Diagnostics to the Hot Star Tau Sco Author: Geneviève de Messières Swarthmore College ‘04 Advised by: David Cohen.

The spectral resolution of x-ray telescopes has improved many hundred-fold over the past decade, enabling us to detect and resolve emission lines in hot.

Chandra Emission Line Diagnostics of  Sco Geneviève de Messières (Swarthmore College ‘04), Carolin Cardamone ( Wellesley College ‘02), David H. Cohen.

AMD Absorption Measure Distribution Evidence for Thermal Instability? By Tomer Holczer Cambridge, MA July 2007.

X-ray Emission from O Stars David Cohen Swarthmore College.

Astrophysics Research Projects: massive star winds, x-ray emission, theoretical models, spectroscopy, laboratory plasma astrophysics David Cohen on leave.

Analysis of Doppler-Broadened X-ray Emission Line Profiles from Hot Stars David Cohen - Swarthmore College with Roban Kramer - Swarthmore College Stanley.

Detection of FIP Effect on Late-type Giants D. Garcia-Alvarez, J.J. Drake, L.Lin, V. Kashyap and B.Ball Smithsonian Astrophysical Observatory Coronal Abundances.

Agreement between X-ray data and magnetically channeled wind shock model of  1 Ori C David Cohen, Marc Gagné for Massive Star research group.

X-ray Spectroscopy of the Radiation-Driven Winds of Massive Stars: Line Profile and Line Ratio Diagnostics David Cohen Swarthmore College.

X-ray Spectroscopy of Laboratory and Astrophysical Plasmas David Cohen Department of Physics and Astronomy Swarthmore College

X-ray Diagnostics and Their Relationship to Magnetic Fields David Cohen Swarthmore College.

X-ray Emission from O Stars David Cohen Swarthmore College.

Lecture 13: Searching for planets orbiting other stars I: Properties of Light 1.How could we study distant habitats remotely ? 2.The nature of light -

A New View of Accretion Shock Structure Nancy S. Brickhouse Harvard-Smithsonian Center for Astrophysics Collaborators: Steve Cranmer, Andrea Dupree, Juan.

X-ray Emission from Massive Stars David Cohen Swarthmore College.

CHAPTER 28 STARS AND GALAXIES

Susan CartwrightOur Evolving Universe1 Atoms and Starlight n Why do the stars shine? l l planets shine by reflected sunlight—but what generates the Sun’s.

Chapter 2 Decoding the Hidden Messages in Starlight

X-ray Spectral Diagnostics of Activity in O and Early-B Stars wind shocks and mass-loss rates David Cohen Swarthmore College.

 Celestial Sphere  Imagine a sphere that surrounds our planet in which all the stars are attached. This sphere is allowed to rotate freely around the.

Astrophysics from Space Lecture 8: Dusty starburst galaxies Prof. Dr. M. Baes (UGent) Prof. Dr. C. Waelkens (KUL) Academic year

Light Years =distance = the speed of light =300,000 km/s =the further you look into the distance, the further back in time you are looking = how far light.

How do colors in a spectrum help us understand stars? Image from

High-Resolution X-ray Spectroscopy of the Accreting Weak-Line T Tauri Star DoAr 21 Victoria Swisher, Eric L. N. Jensen, David H. Cohen (Swarthmore College),

X-ray Diagnostics and Their Relationship to Magnetic Fields David Cohen Swarthmore College.

Post Processing of ZEUS MHD Simulations of Young, Hot Stars Stephen V. St.Vincent and David H. Cohen Swarthmore College Department of Physics & Astronomy.

X-ray Observations of Stars Rachel Osten University of Maryland, NASA/GSFC (The highest spatial resolution X-ray observation of a star!)

Diagnosing the Shock from Accretion onto a Young Star Nancy S. Brickhouse Harvard-Smithsonian Center for Astrophysics Collaborators: Steve Cranmer, Moritz.

X-ray Diagnostics and Their Relationship to Magnetic Fields David Cohen Swarthmore College.

Electromagnetic Spectrum. The Universe The Big Bang forms the universe….. The energy creates stars. Gravity pulls stars together into Galaxies. The stars.

Chandra X-Ray Spectroscopy of DoAr 21: The Youngest PMS Star with a High-Resolution Grating Spectrum The High Energy Grating Spectrum of DoAr 21, binned.

Student-Faculty Astronomy Research at Swarthmore: Or…doing astronomy research when the Sun is up Professor David Cohen with Victoria Swisher ( ‘ 06), Micah.

X-ray Group Meeting Observations of Hot Star Winds Absorption Spectroscopy, Radiation (line-) Driving, and X-rays 9 February 2001 David Cohen Allison Adelman.

Ay 123 Lecture I - Physical Properties 10  as = 10% 10  as/yr = ESA Gaia mission: a revolution in 3-D mapping of our Galaxy.

Galaxies with Active Nuclei Chapter 14:. Active Galaxies Galaxies with extremely violent energy release in their nuclei (pl. of nucleus).  “active galactic.

Conclusions The prototype  Pup (O4 I) has X-ray emission line profiles consistent with a simple spherically symmetric wind shock model. What can lead.

2.4 Studying the Sun. Electromagnetic Radiation  The visible light we see is only a fraction of energy coming from various objects  Most of what we.

Astronomy. I. Early Astronomers  Ptolemy: (140 yr)  A Greek astronomer theorized the model of the universe. The Ptolemaic theory suggested that the.

X-ray Line Profile Diagnostics of Shock Heated Stellar Winds Roban H. Kramer 1,2, Stephanie K. Tonnesen 1, David H. Cohen 1,2, Stanley P. Owocki 3, Asif.

The impact of magnetic turbulence spectrum on particle acceleration in SNR IC443 I.Telezhinsky 1,2, A.Wilhelm 1,2, R.Brose 1,3, M.Pohl 1,2, B.Humensky.

Resolved X-ray Line Profiles from O Stars as a Diagnostic of Wind Mass Loss David Cohen Department of Physics & Astronomy Swarthmore College Jon Sundqvist.

Siderius Nuntius… Light and the Science of Astronomy.

Chapter 24 Video Field Trip: Fireball Write down five facts from the video!

The Young Magnetic O Star  1 Ori C: Multi-phase Chandra High-Resolution Grating Spectra Mary Oksala, Marc Gagné (West Chester University), David Cohen,

Oct. 16, Review: Continuum vs. Line spectra of Stars Blackbody continuum spectrum (Wien’s Law and S-B Law) give color and thus temperature, and.

4. Complex Knowledge: demonstrations of learning that go aboveand above and beyond what was explicitly taught. 3. Knowledge: meeting the learning goals.

High Energy Observational Astrophysics. 1 Processes that emit X-rays and Gamma rays.

Unveiling the Secrets of the Stars. Hot objects emit radiation (light). The hotter they are the more radiation they emit and the higher energy of that.

Spectroscopy Lecture.

Chandra Science Highlights

Presentation transcript:

Trends in the Chandra X-Ray Spectra of O and Early B Stars June 24, 2008

Spectra of Stars We know that spectra result from physical processes within stars. They often reflect physical properties of the stars that created them. ex. Optical Spectra

X-Ray Spectra of O and Early B Stars The spectra on the left are a representative sampling of O and early B star spectra, with earlier spectral types at top. The spectra were taken on the Chandra X- Ray telescope using the high energy transmission grating (HETG) on the advanced camera for imaging spectroscopy (ACIS). Nolan Walborn suggested in a 2006 paper that these spectra may reveal a temperature trend similar to that observed for optical spectra. I will be looking for evidence that tends to confirm or disprove this hypothesis.

X-Ray Production in Hot Stars X-Ray emission arises in the stellar winds of these stars. The stellar winds are radiatively driven. The line-driven stellar winds are inherently unstable. Shocks in the wind arise from the instability and produce x-rays.

X-Ray Spectra and Temperature Line strength ratios Differential Emission Measure dEM= n e n H dV In a plasma with a single well-defined temperature, or D(T)= n e (T)n H (T)(dV/d logT) in a plasma with a temperature distribution.

Stars and Parameters HD93129AB O2 If* + (2x) O3.5 V((f + )) T eff = K R= 20 R sun M=120 M sun v inf = 3200 km/s dM/dt = 1.8 * M sun /yr Xi Persei O7.5 III(n)((f)) T eff = K R= 12 R sun M=34 M sun v inf = 2450 km/s dM/dt = 2.0 * M sun /yr Delta Orionis O9.5 II + B0.5 III T eff = K R= 17 R sun M=23 M sun v inf = 2000 km/s dM/dt = 1.07 * M sun /yr

Silicon XIV/Silicon XIII Ratios HD93129AB 0.05 ± 0.02 Xi Persei 0.05 ± 0.02 Delta Orionis 0.21 ± 0.06

Magnesium XIV/Magnesium XIII Ratios Xi Persei 0.12 ± 0.02 HD93129AB 0.27 ± 0.04 Delta Orionis 0.24 ± 0.03

Conclusions (for now) Line ratios of stars in our sample seem to have little to do with effective temperature. This tends to disprove Walborn’s suggestion that the trend in the spectrum is temperature- related. However, there does appear to be some slight tendency for individual lines to become broader and more blueshifted in the hotter stars.

Some Directions for Research Continue to measure line ratios in more stars. Possibly explore measuring line ratios for other elements. Look into measuring emission measures for our sample stars as another probe of temperature.