EVIDENCE FOR THE WHITE DWARF NATURE OF MIRA B

@article{Sokoloski2010EVIDENCEFT,
  title={EVIDENCE FOR THE WHITE DWARF NATURE OF MIRA B},
  author={J. L. Sokoloski and Lars Bildsten},
  journal={The Astrophysical Journal},
  year={2010},
  volume={723},
  pages={1188-1194}
}
The nature of the accreting companion to Mira?the prototypical pulsating asymptotic giant branch star?has been a matter of debate for more than 25?years. Here, we use a quantitative analysis of the rapid optical brightness variations from this companion, Mira B, which we observed with the Nickel Telescope at Lick Observatory, to show that it is a white dwarf (WD). The amplitude of aperiodic optical variations on timescales of minutes to tens of minutes (0.2?mag) is consistent with that of… 

Figures and Tables from this paper

The Nucleus of the Planetary Nebula EGB 6 as a Post-Mira Binary
EGB 6 is a faint, large, ancient planetary nebula (PN). Its central star, a hot DAOZ white dwarf (WD), is a prototype of a rare class of PN nuclei associated with dense, compact emission-line knots.
X-Ray Emissions from Accreting White Dwarfs: A Review
Interacting binaries in which a white dwarf accretes material from a companion - cataclysmic variables (CVs) in which the mass donor is a Roche-lobe filling star on or near the main sequence, and
Red giant pulsations from the suspected symbiotic star StHA 169 detected in Kepler data
We present Kepler and Swift observations of StHa 169 which is currently classified as a symbiotic binary. The Kepler light curve shows quasi periodic behaviour with a mean period of 34 d and an
INFRARED SPECTROSCOPY OF SYMBIOTIC STARS. IX. D-TYPE SYMBIOTIC NOVAE
Time-series spectra of the near-infrared 1.6 {mu}m region have been obtained for five of the six known D-type symbiotic novae. The spectra map the pulsation kinematics of the Mira component in the
Morphology and kinematics of the gas envelope of Mira Ceti
Observations of 12CO(3-2) emission of the circumbinary envelope of Mira Ceti, made by ALMA are analysed. The observed Doppler velocity distribution is made of three components: a blue-shifted
New Measurements of the Radio Photosphere of Mira Based on Data from the JVLA and ALMA
We present new measurements of the millimeter wavelength continuum emission from the long period variable Mira (oCeti) at frequencies of 46, 96, and 229 GHz ( 7 l » , 3, and 1 mm) based on
WIND-ACCRETION DISKS IN WIDE BINARIES, SECOND-GENERATION PROTOPLANETARY DISKS, AND ACCRETION ONTO WHITE DWARFS
Mass transfer from an evolved donor star to its binary companion is a standard feature of stellar evolution in binaries. In wide binaries, the companion star captures some of the mass ejected in a
Dust around the Cool Component of D-Type Symbiotic Binaries
D type symbiotic binaries are an excellent astrophysical laboratory for investigation of the dust properties and dust formation under the influence of theMira stellar wind and nova activity and of
Flickering in AGB stars: probing the nature of accreting companions
Binary companions to asymptotic giant branch (AGB) stars are an important aspect of their evolution. Few AGB companions have been detected, and in most cases it is difficult to distinguish between
Is Mira a magneto-dusty rotator?
We investigate the possibility that a magnetic field may be present in the star $o-$Ceti (hereafter, Mira) and that the field plays a role in the star's mass loss. The model presented here is an
...
1
2
3
4
...

References

SHOWING 1-10 OF 62 REFERENCES
Born-Again Protoplanetary Disk around Mira B
The Mira AB system is a nearby (~107 pc) example of a wind accreting binary star system. In this class of system, the wind from a mass-losing red giant star (Mira A) is accreted onto a companion
Measuring White Dwarf Accretion Rates via Their Effective Temperatures
Our previous theoretical study of the impact of an accreting envelope on the thermal state of an underlying white dwarf (WD) has yielded equilibrium core temperatures, classical nova ignition masses,
Theoretical Modeling of the Thermal State of Accreting White Dwarfs Undergoing Classical Nova Cycles
White dwarfs (WDs) experience a thermal renaissance when they receive mass from a stellar companion in a binary. For accretion rates of less than 10-8 M☉ yr-1, the freshly accumulated hydrogen/helium
The ultraviolet spectrum of the companion of Mira (omicron Ceti) : observational evidence for a disk formed by wind accretion.
Extensive spectroscopic observations with IUE of the companion of Mira (omicron Ceti B) are presented. It is shown that the UV continuum observed with IUE is exclusively due to Mira B at Mira A
A search for rapid photometric variability in symbiotic binaries
We report on our survey for rapid (time scale of minutes) photometric variability in symbiotic binaries. These binaries are becoming an increasingly important place to study accretion onto white
THE NATURE OF THE HARD X-RAY-EMITTING SYMBIOTIC STAR RT CRU
We describe Chandra High Energy Transmission Grating Spectrometer observations of RT Cru, the first of a new subclass of symbiotic stars that appear to contain white dwarfs (WDs) capable of producing
First Hubble Space Telescope Observations of Mira AB Wind-accreting Binary System
The Mira AB system belongs to a class of detached binaries in which a compact object accretes mass from the wind of a cool giant or supergiant. This system provides a unique laboratory for detailed
White dwarfs in cataclysmic variables.
Prior to the last 15 years, the literature on cataclysmic variables (CVs) contained little on the properties of the underlying white dwarf accreter other than estimates of their masses. They were
A turbulent wake as a tracer of 30,000 years of Mira’s mass loss history
TLDR
The discovery of an ultraviolet-emitting bow shock and turbulent wake extending over 2 degrees on the sky, arising from Mira’s large space velocity and the interaction between its wind and the ISM.
Spreading of Accreted Material on White Dwarfs
When a white dwarf (WD) is weakly magnetized and its accretion disk is thin, accreted material first reaches the WD's surface at its equator. This matter slows its orbit as it comes into corotation
...
1
2
3
4
5
...