Cataclysmic Variables in K2 Paula Szkody ( U Washington ), Zhibin Dai ( Yunnan Obs ), Peter Garnavich ( Notre Dame ), Mark Kennedy ( ND+Ireland )

Slides:

Advertisements

Similar presentations

Introduction to Binary Stars Steve B. Howell NOAO.

Advertisements

Cataclysmic Variables in the AAVSO Observing Program Janet A. Mattei Kerriann H. Malatesta AAVSO Second HEA Workshop July 4-5, 2002, Waikoloa Beach, Hawaii.

Makoto Uemura (Kyoto University : VSNET team)

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

The First MMT Science Symposium In recognition of the service of J.T. Williams The MMT’s Role in Understanding Magnetic Accretion Binaries June 15, 2006.

ASTR Fall Semester Joel E. Tohline, Alumni Professor Office: 247 Nicholson Hall [Slides from Lecture17]

Light Curves of the Dwarf Nova U Gem: A Diagnostic of Accretion Disk Evolution Larry Molnar Calvin College Grand Rapids, Michigan.

EF Eri: Onset of Chromospheric Activity in the Sub-Stellar Secondary

An ancient nova shell around the dwarf nova Z Camelopardalis Michael M. Shara, et al. 2007, Nature, Vol March 鹿豹星座.

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

Cataclysmic Variable Stars Nataliya Ostrova Astronomical observatory of the Odessa National University, T.G. Shevchenko Park, Odessa,

RXTE Observations of Cataclysmic Variables and Symbiotic Stars Koji Mukai NASA/GSFC/CRESST and UMBC.

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

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

Multicolour photometry of unusual dwarf nova star HS Golysheva P., Shugarov, S., Katysheva N., Chochol D. Sternberg Astronomical Institute, Moscow.

Variable Stars: the Partially Known and the Totally Unknown The Eventful Universe March 18 Paula Szkody + many.

R. Hudec, V. Šimon F. Munz, J. Štrobl, P. Kubánek, P. Sobotka, R. Urban Astronomical Institute, Academy of Sciences Ondrejov, Czech Republic & ISDC,

Pulsating WD Paula Szkody, Anjum Mukadam, Boris Gaensicke, Arne Henden + AAVSO, Atsuko Nitta, Ed Sion, Dean Townsley Wild Stars March 16, 2009 Tantalizing.

The Downside of EF Eridani Frederick M. Walter Stony Brook University There’ve been strange things done to this former sun by the nearby white dwarf star.

Time Series Photometry; Some Musings Steve B. Howell, NASA Ames Research Center.

Variable Stars clues: timescale, amplitude, light curve shape, spectrum Eclipsing: Algol ß Lyr W UMa B8-M (hrs-days) B8-G3 F0-K0 (hrs) Eruptive: single.

Vadim Burwitz X-ray Grating Spectroscopy, Cambridge, MA, July 12, 2007 The complex and variable X-ray spectra of the super-soft source RXJ Vadim.

Variable Stars clues: timescale, amplitude, light curve shape, spectrum Eclipsing: Algol ß Lyr W UMa B8-M (hrs-days) B8-G3 F0-K0 (hrs)‏ Eruptive: single.

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

Presented by Anna Hourihane Searching for Dwarf Novae in Globular Clusters Anna Hourihane a, Paul Callanan a and Adrienne Cool b a Department of Physics,

ASTR377: A six week marathon through the firmament by Orsola De Marco Office: E7A 316 Phone: Week 6, May 24-27, 2009.

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.

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

(University of Texas at El Paso) (New Mexico State University at Doña Ana) Radio Observations of Cataclysmic Variables Paul A. Mason (University of Texas.

Basics of Cataclysmic Variables iPTF Summer School August 28, 2014 Paula Szkody U of Washington.

Cataclysmic variables as hard X-ray emitters seen by INTEGRAL The X-ray Universe 2008, Granada, Spain, May R. Gális 1,2, R. Hudec 1, F. Münz 3, M.

Populations of Galactic X-ray (compact) sources visible to Spectrum-RG Revnivtsev M., Space Research Institute; Moscow, Russia.

The SW Sextantis stars and the evolution of cataclysmic variables

V. Simon, G. Pizzichini, R. Hudec The optical long-term activity of the high-energy sources: Perspectives for ESA Gaia v 1 Astronomical Institute, The.

Constraints on progenitors of Classical Novae in M31 Ákos Bogdán & Marat Gilfanov MPA, Garching 17 th European White Dwarf Workshop 18/08/2010.

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

Aiying ZHOU 周爱英 Beijing National Astronomical Observatories, CAS —— Several Observational Aspects.

Mean period of pulsating white dwarfs as a spectroscopy-independent thermometer Anjum S. Mukadam, University of Washington Collaborators: M. H. Montgomery.

The asynchronous polar V1432 Aquilae and its path back to synchronism The CBA consortium David Boyd, Joseph Patterson, William Allen, Greg Bolt, Michel.

C R I M E A Activity of five WZ Sge- type systems in a few years after their outbrsts E.P. Pavlenko, O.I. Antoniuk, K.A. Antoniuk, D.A. Samsonov, A.V.

New Close Binary Systems (WD + MS) from SDSS (DR 5) And the Search for Magnetic White Dwarfs in Cataclysmic Variable Progenitor Systems Nicole Silvestri.

Binary millisecond X-ray pulsars Department of Physics University College Cork Paul Callanan and Mark Reynolds Alexei Filippenko, Department of Astronomy,

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

The Photometric Study of New SU UMA Dwarf Nova SDSS J16 h 25 m 20 s +12 o 03’08”. The Scargle-Lomb periodogram determined by observations at superoutburst.

1. INTRODUCTION As the brightest dwarf nova and one of the brightest cataclysmic variables of any kind, SS Cygni has been extensively observed. Its outbursts,

R. Hudec, F. Munz, J. Štrobl, P. Kubánek, P. Sobotka, R. Urban Astronomical Institute, Academy of Sciences Ondrejov, Czech Republic & ISDC, Versoix,

August 28, 2014PTF Summer School Novae in Local Group Galaxies, but really just Andromeda A. W. Shafter San Diego State University Modified and delivered.

The Radio Millisecond Pulsar PSR J : A Link to Low-Mass X-Ray Binaries Slavko Bogdanov.

(University of Texas at El Paso) (New Mexico State University at Doña Ana) Radio Observations of Cataclysmic Variables Paul A. Mason (University of Texas.

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

Nature of X-ray transients in the Magellanic Clouds : (Be/X-ray pulsars, and Supersoft sources) Andry RAJOELIMANANA 1, 2 ‏ Supervisor : Prof Phil CHARLES.

Cataclysmic Variables: A Perfect Testbed for Variability Brokering Paula Szkody University of Washington Santa Barbara May 13, 2015.

K.Byckling, J. Osborne, G. Wynn, A. Beardmore, V. Braito (UoL), K. Mukai (NASA/GSFC), R. West (UoL) March 15-19, 2009 Wild stars in the Old West Tucson,

Classical Novae on a Helium White Dwarf Irit Idan (Technion) Lars Bildsten ((KITP, UCSB) Ken Shen (UCSB)

Bled, March 2008Anna Sponselli AQUEYE: SCIENTIFIC TARGETS.

Vojtech Simon v X-ray monitoring of cataclysmic variables – dependence on the instruments Talk: International Workshop on Astronomical X-Ray Optics, Prague,

The APO 3.5m at UW Suzanne Hawley University of Washington Many scientific programs including: –chemical abundance studies (Wallerstein) –planetary nebulae.

Formation of Redback and Black Widow Binary Millisecond Pulsars

Three Challenges to standard assumptions 9/27/13Rosanne Di Stefano, 27 September 2013.

Time Domain Astrophysics Stephen Potter South African Astronomical Observatory.

Transient Identification and Classification with WISE Doug Hoffman R. Cutri & T. Jarrett The Eventful Universe, 2010.

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

The OmegaWhite Survey Paul Groot Radboud Universiteit Nijmegen.

Very hard X-ray binaries containing white dwarfs

Lessons Learned from Past/Ongoing Sky Survey Followup

Mariko KATO (Keio Univ., Japan) collaboration with

Observations of compact binaries using XMM-Newton

X-ray Grating Spectroscopy of Cataclysmic Variables

NEAR-CONTACT BINARY V836 Cygni Çanakkale, 2004

The Link Between Underluminous Supernovae Explosions, Gravitational Waves and Extremely Low Mass White Dwarfs Alex Gianninas Mukremin Kilic, Warren Brown,

Presentation transcript:

Cataclysmic Variables in K2 Paula Szkody ( U Washington ), Zhibin Dai ( Yunnan Obs ), Peter Garnavich ( Notre Dame ), Mark Kennedy ( ND+Ireland )

A Cataclysmic Variable : is a close binary system has a white dwarf primary has a cool low mass secondary actively transfers mass

Disk System Polar Intermediate Polar LARP CV Types Steve Howell outbursts high,low states mostly high state all low state

Examples from CSS sampling rate Low accretion rateHigh accretion rate

Kepler field sampling V344 Lyr Cannizzo et al. 2012, ApJ, 747,117

K2 Advantages for CVs: Details of outbursts (disks) Orbital periodicities (evolution) Orbital accretion changes (spots) Spin Periods of WDs in IPs (curtains) Samples different locations in galaxy

Outbursts--tests of disk theory Shapes-decline, peak,width Recurrence times Pre-cursors

K2-0

 parabola-like decay of outburst  linear and slow transit between outburst and quiescence.  quiescence covering at least 28 days shows typical flickering behavior. ~ 1 mag ~ 4.5 days 28 days USNO Dwarf nova K2-0 Changes in shape during late decline Flickering at quiesence

 The ends of normal outbursts are different. A smooth and fast variation is shown in UV Gem, while a rough and slow linear transit with duration of 4.5 days in USNO.  V344 Lyr is a SU UMa type dwarf nova with an orbital period of 2.1 hr, same as UV Gem. V344 Lyr 2.1 hr UV Gem USNO From Kepler data Cannizzo et al. 2012

K2-1 TW Vir Pre-cursor

K2-1 RXJ1112

MLS MLS K2-4

MLS (SDSS ) K2-4

e.g. V1159 Ori – 45 day supercycle ( Szkody et al. 1999, ApJ, 521, 362 ) Is MLS0359 a rare supercycle system?

Orbital Variations Eclipses Hot spots Reflection effects

P=1.23 d eclipses 5 days K2-2

K2-0 SDSSJ

7.78 hrs 3.89 hrs SDSSJ0632

K2-1 WD DA+dMe Pre-CV?

Intermediate Polars WD spin period Amplitudes in opt/vs UV Variability over time

K2-3 Intermediate Polar FO Aqr 1 day of SC observations P orb = 4.85 hr P spin = 20.9 min

P orb P spin

FO Aqr

Amplitude of spin lowest at phase 0, highest at 0.7

Summary K2 LC great for testing disk, outburst theories, providing orbital periods, accretion changes during quiescence K2 SC vital for eclipse, spin studies and their variations on daily, weekly, monthly timescales