PCEBs from the SDSS testing disrupted magnetic braking Matthias Schreiber Tucson, March-2009 Boris T. Gaensicke, John Southworth, S. Stylianos (Warwick)

Slides:

Advertisements

Similar presentations

The Secondary Stars of Cataclysmic Variables Christian Knigge arXiv: v2 reporter:ShaoYong.

Advertisements

X-ray pulsars in wind-fed accretion systems 王伟 (NAOC) July 2009, Pulsar Summer School Beijing.

SDSS finds the period minimum spike Boris Gänsicke John Southworth John Thorstensen M Dillon, P Rodríguez-Gil, A Aungwerojwit, TR Marsh, P Szkody, SCC.

Lecture 26: The Bizarre Stellar Graveyard: White Dwarfs and Neutron Stars.

Small is Beautiful: Cataclysmic Variables from the SDSS John Southworth Boris Gänsicke Tom Marsh + many others.

Christian Knigge University of Southampton School of Physics & Astronoy P. Marenfeld and NOAO/AURA/NSF Christian Knigge University of Southampton Low-Mass.

AS 4002 Star Formation & Plasma Astrophysics Protostellar spin evolution Solve equation of motion numerically Use a stellar evolution code (Eggleton 1992)

Christian Knigge University of Southampton School of Physics & Astronoy Disk Stability vs Close Binary Evolution Rob Hynes (LSU) Christian Knigge University.

Accretion Processes in GRBs Andrew King Theoretical Astrophysics Group, University of Leicester, UK Venice 2006.

Angular momentum evolution of low-mass stars The critical role of the magnetic field Jérôme Bouvier.

Accretion in Binaries Two paths for accretion –Roche-lobe overflow –Wind-fed accretion Classes of X-ray binaries –Low-mass (BH and NS) –High-mass (BH and.

On the Roche Lobe Overflow Reporter: Wang Chen 12/02/2014 Reference: N. Ivanova, v1.

AS 3004 Stellar Dynamics Mass transfer in binary systems Mass transfer occurs when –star expands to fill Roche-lobe –due to stellar evolution –orbit, and.

Neutron Stars Chandrasekhar limit on white dwarf mass Supernova explosions –Formation of elements (R, S process) –Neutron stars –Pulsars Formation of X-Ray.

HOW MANY NEUTRON STARS ARE BORN RAPIDLY ROTATING? HOW MANY NEUTRON STARS ARE BORN RAPIDLY ROTATING? NIKOLAOS STERGIOULAS DEPARTMENT OF PHYSICS ARISTOTLE.

Mass Loss and Evolution of Low-Mass X-ray Binaries Xiang-Dong Li Department of Astronomy Nanjing University

VLT spectroscopy of SDSS cataclysmic variables John Southworth Boris Gänsicke Tom Marsh.

New Insights on the origin of Magnetic Fields in White Dwarfs Dayal Wickramasinghe and Lilia Ferrario Australian National University Canberra.

Compact Objects Astronomy 315 Professor Lee Carkner Lecture 15.

Marc Pinsonneault (OSU).  New Era in Astronomy  Seismology  Large Surveys  We can now measure things which have been assumed in stellar modeling 

A Review of Magnetic Activity in Sun-like stars Magnetic Stars Seminar Oct. 30, 2002.

18 Dark Matter Join me on the Dark Side. 18 Goals The Universe is expanding. Will it expand forever? Depends on mass? How do we know the mass of the universe?

Theoretical Studies of X-Ray Binaries in Clusters Vicky Kalogera MODEST-6 ExtraGalactic only…

Mass Determinations of Short Period CV Donors Authors: Christopher D.J. Savoury*, S.P Littlefair*, V.S. Dhillion*, T.R. Marsh #, B.T. Gänsicke #, *The.

Spin angular momentum evolution of the long-period Algols Dervişoğlu, A.; Tout, Christopher A.; Ibanoğlu, C. arXiv:

Magnetism in Herbig Ae/Be stars and the link to the Ap/Bp stars E. Alecian, C. Catala, G.A. Wade, C. Folsom, J. Grunhut, J.-F. Donati, P. Petit, S. Bagnulo,

He star evolutionary channel to intermediate-mass binary pulsars with a short-orbital-period Chen Wen-Cong School of Physics, Peking University Department.

Transitional Millisecond pulsars as accretion probes

Ecology of Blue Stragglers: Closing Thoughts and Discussion.

INAF, Osservatorio Astronomico di Roma XI Advanced School of Astrophysics, Brazil, 1-6 September 2002.

The SW Sextantis stars and the evolution of cataclysmic variables

Christian Knigge University of Southampton School of Physics & Astronoy The Secondary Stars of Cataclysmic Variables P. Marenfeld and NOAO/AURA/NSF Christian.

Physics 681: Solar Physics and Instrumentation – Lecture 19 Carsten Denker NJIT Physics Department Center for Solar–Terrestrial Research.

Cataclysmic Variables in the UV D.de Martino INAF-Osservatorio Astronomico di Capodimonte Napoli & B.T. Gaensicke (Warwick), K.Long (STScI), T.R.Marsh.

Lars Bildsten Kavli Institute for Theoretical Physics University of California Santa Barbara Unusual Binaries made via Interactions.

CV and pre-CV populations in the SDSS era Ulrich Kolb with Phil Davis (OU), Bart Willems (NWU)

Cosmological Galaxy Formation

A Test for the Disruption of Magnetic Braking in Cataclysmic Variable Evolution P. Davis 1, U. Kolb 1, B. Willems 2, B. T. Gänsicke 3 1 Department of Physics.

A few Challenges in massive star evolution ROTATIONMAGNETIC FIELD MULTIPLICITY How do these distributions vary with metallicity? How do these distributions.

Precession during merger R. O’Shaughnessy (UWM) J. Healy, L. London, D. Shoemaker (Georgia Tech) Midwest Relativity Meeting, Chicago arXiv:

INTRODUCTION OVERVIEW  Classical Novae (CNe) are thought to occur in binary systems known as Cataclysmic Variables (CV’s).  CV’s are close, interacting.

Radio Observations of X-ray Binaries : Solitary and Binary Millisecond Pulsars Jeong-Sook Kim 1 & Soon-Wook Kim 2  Department of Space Science and Astronomy.

Dynamical formation of LMXBs in the inner bulge of M31 by Rasmus Voss with Marat Gilfanov X-rays from nearby galaxies ESAC September 2007.

Where are the Accreting Helium White Dwarfs?? Drawing by T. Piro.

From an evolutionary point of view Selma de Mink Utrecht University Lorentz Center Workshop “Stellar Mergers” Ines Brott (Utrecht), Matteo Cantiello (Utrecht),

Constraining close binaries evolution with SDSS/SEGUE: a representative sample of white dwarf/main sequence binaries Matthias Schreiber ESO, May 4th, 2006.

Magnetism and Rotation in Herbig Ae/Be stars E. Alecian Laboratoire d’Astrophysique de l’Observatoire de Grenoble In collaboration with G.A. Wade, C. Catala,

Orbital evolution of compact Black-hole binaries and white dwarf binaries Wencong Chen Astro-ph/ Astro-ph/

After the Supernova: Pulsars Melissa Anholm University of Wisconsin-Milwaukee 29 September, 2008.

Evolutionary Sequences For Low- And-Intermediate-Mass X-Ray Binaries Ph. Podsiadlowski S. Rappaport E. D. Pfahl.

The Herbig Ae/Be stars: what we have learnt with ESPaDOnS E. Alecian, G.A. Wade, C. Catala, C. Folsom, J. Grunhut, J.-F. Donati, P. Petit, S. Bagnulo,

On the other hand.... CDM simulations consistently produce halos that are cusped at the center. This has been known since the 1980’s, and has been popularized.

Rotation Among High Mass Stars: A Link to the Star Formation Process? S. Wolff and S. Strom National Optical Astronomy Observatory.

14 Dark Matter Join me on the Dark Side. 14 Goals Why do we think there is dark matter? Where do we think it is? How much is there?

Formation of Redback and Black Widow Binary Millisecond Pulsars

Outrageous OutburstsWild Stars in the Old West II, Tucson, Arizona, March 2009 Outrageous Outbursts: Accretion Disc Formation and Stability in Long.

ASTR112 The Galaxy Lecture 12 Prof. John Hearnshaw 16. Evolution of the Galaxy 16.1 Star formation 16.2 Exchange of material between stars and ISM 16.3.

Binary Origin of Blue Stragglers Xuefei CHEN Yunnan Observatory, CHINA.

FOUR NEW ECLIPSING CATACLYSMIC VARIABLES FROM THE SDSS John Southworth and Boris Gänsicke Department of Physics, University of Warwick, UK

The Minimum Mass Ratio for Contact Close Binary

A cloud of gas falling towards the central black hole in the Milky Way. Jordi Miralda Escudé ICREA, Institut de Ciències del Cosmos University of Barcelona.

THEORY OF MERIDIONAL FLOW AND DIFFERENTIAL ROTATION

Predicting the BRAING INDEX OF INTERMITTENT AND NULLING PULSARS

Basic Properties By Dr. Lohse, University of Berlin

Progenitors of long GRBs

Signatures of formation mechanisms in the multiple-star statistics

Dark Matter Join me on the Dark Side.

Dark Matter Join me on the Dark Side.

Evolution of X-ray Binaries and the Formation of Binary Pulsars

ASTEROSEISMOLOGY OF LATE STAGES OF STELLAR EVOLUTION

Presentation transcript:

PCEBs from the SDSS testing disrupted magnetic braking Matthias Schreiber Tucson, March-2009 Boris T. Gaensicke, John Southworth, S. Stylianos (Warwick) A. Rebassa-Mansergas (Valparaiso) M. Zorotovic-Fiebig, C. Tappert (PUC Santiago) L. Schmidtobreik (ESO) A. D. Schwope, A. Nebot Gomez-Moran (AIP)

The orbital period distribution of CVs Ritter & Kolb (2003)

1983: Disrupted magnetic braking (DMB) Paczynski & Sienkiewicz; Spruit & Ritter; Rappaport et al. (1983) Two angular momentum loss mechanisms: magnetic wind braking & gravitational radiation MWB+GRGR

DMB: believe it or not Cons: -Spin down rates of low-mass stars in open clusters (Sills et al. 2000) -Large scale magnetic fields in fully convective stars (Donati et al. 2006) Pros: -Mean mass transfer rates of CVs (Townsley & Gaensicke 2008) -Donor star mass-radius relation (e.g. Knigge 2006)

Predicted PCEB fractions Politano & Weiler (2006)

WDMS and PCEBs from the SDSS -SEGUE and SDSS identified ~2000 WDMS -We followed-up PCEBs identified (~39%) -54 orbital periods measured (see next talk)

PCEB fraction versus secondary spectral type

PCEB fraction versus secondary mass

Comparing predictions and observations Politano & Weiler (2006)

-fast fully convective rotators in old field stars -not a single early M fast rotator (Reiners et al. 2008) -change in the magnetic field topology at ~M3.5 (Donati et al. 2008) Disrupted braking in single old field M dwarfs

Conclusion Disrupted braking confirmed!

Remaining questions Why does braking get disrupted? How strong is AML below the gap? Why is it different in young stars?

For questions

Gemini PCEB identifications (2007B, 2008A)

3 good reasons to believe in DMB -Mean mass transfer rates of CVs (Townsley & Gaensicke 2008) -Expanded secondaries above the gap (e.g. Knigge et al. 2006)

Selection effects Bias towards short orbital periods Bias towards low mass secondaries

Disrupted braking in single field M dwarfs?