A Self-consistent Model for a Full Cycle of Recurrent Novae—Wind Mass-loss Rate and X-Ray Luminosity

The radio emission from supernovae provides a direct probe of a supernova’s circumstellar environment, which presumably was established by mass-loss episodes in the late stages of the progenitor’s presupernova evolution. The observed synchrotron emission is generated by the SN shock interacting with the relatively high-density circumstellar medium which has been fully ionized and heated by the initial UV/X-ray flash. The study of radio supernovae therefore provides many clues to and constraints on stellar evolution. We will present the recent results on several cases, including SN 1980K, whose recent abrupt decline provides us with a stringent constraint on the progenitor’s initial mass; SN 1993J, for which the profile of the wind matter supports the picture of the progenitor’s evolution in an interacting binary system; and SN 1979C, where a clear change in presupernova mass-loss rate occurred about 104 years before explosion. Other examples, such as SNe 19941 and 1996cb, will also be discussed.

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Mass loss via solar wind and coronal mass ejections during solar cycles 23 and 24

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1001 ◽

2019 ◽

Vol 486 (4) ◽

pp. 4671-4685 ◽

Cited By ~ 5

Author(s):

Wageesh Mishra ◽

Nandita Srivastava ◽

Yuming Wang ◽

Zavkiddin Mirtoshev ◽

Jie Zhang ◽

...

Keyword(s):

Solar Wind ◽

Mass Loss ◽

Sunspot Number ◽

Loss Rate ◽

Mass Loss Rate ◽

Occurrence Rate ◽

The Sun ◽

Solar Cycles ◽

X Ray ◽

X Ray Background

ABSTRACT Similar to the Sun, other stars shed mass and magnetic flux via ubiquitous quasi-steady wind and episodic stellar coronal mass ejections (CMEs). We investigate the mass loss rate via solar wind and CMEs as a function of solar magnetic variability represented in terms of sunspot number and solar X-ray background luminosity. We estimate the contribution of CMEs to the total solar wind mass flux in the ecliptic and beyond, and its variation over different phases of the solar activity cycles. The study exploits the number of sunspots observed, coronagraphic observations of CMEs near the Sun by SOHO/LASCO, in situ observations of the solar wind at 1 AU by WIND, and GOES X-ray flux during solar cycles 23 and 24. We note that the X-ray background luminosity, occurrence rate of CMEs and ICMEs, solar wind mass flux, and associated mass loss rates from the Sun do not decrease as strongly as the sunspot number from the maximum of solar cycle 23 to the next maximum. Our study confirms a true physical increase in CME activity relative to the sunspot number in cycle 24. We show that the CME occurrence rate and associated mass loss rate can be better predicted by X-ray background luminosity than the sunspot number. The solar wind mass loss rate which is an order of magnitude more than the CME mass loss rate shows no obvious dependency on cyclic variation in sunspot number and solar X-ray background luminosity. These results have implications for the study of solar-type stars.

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On the thermal atmospheric escape of π Men c

Астрономия и исследование космического пространства: Всероссийская с международным участием научная конференция студентов и молодых ученых, посвященная памяти Полины Евгеньевны Захаровой ◽

10.15826/b978-5-7996-3229-8.28 ◽

2021 ◽

Author(s):

E. S. Kalinicheva ◽

◽

V. I. Shematovich ◽

Ya. N. Pavlyuchenkov ◽

◽

...

Keyword(s):

Mass Loss ◽

Loss Rate ◽

Mass Loss Rate ◽

Upper Atmosphere ◽

One Dimensional ◽

Atmospheric Escape ◽

Self Consistent ◽

Atmospheric Mass ◽

Suprathermal Particles

In this work we present the results of the modeling of exoplanet pi Men c upper atmosphere, produced using the previously developed one-dimensional self-consistent aeronomic model. The model used takes into account the contribution of suprathermal particles, which significantly refines the heating function of the atmosphere. The hight profiles of temperature, velocity and density were obtained, the atmospheric mass-loss rate was calculated. The presence of two hight-scales in the structure of the atmosphere was found: the first corresponds to a relatively dense stationary atmosphere, the second to a more rarefied corona.

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In hot pursuit of the hidden companion of η Carinae: an X-ray determination of the wind parameters

Symposium - International Astronomical Union ◽

10.1017/s0074180900212102 ◽

2003 ◽

Vol 212 ◽

pp. 218-219

Author(s):

Julian M. Pittard ◽

Michael F. Corcoran

Keyword(s):

Binary System ◽

Mass Loss ◽

Loss Rate ◽

Mass Loss Rate ◽

X Ray ◽

The Galaxy ◽

Binary Hypothesis ◽

Η Car

We perform X-ray spectral fits to a recently obtained Chandra grating spectrum of η Carinae, one of the most massive and powerful stars in the Galaxy and which is strongly suspected to be a colliding wind binary system. The good fit that we obtain gives us further confidence in the binary hypothesis, and we find M ≈ 2.5 × 10–4 M⊙ yr–1 for the mass loss rate of η Car.

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X-ray spectral diagnostics of activity in massive stars

Proceedings of the International Astronomical Union ◽

10.1017/s1743921311010763 ◽

2010 ◽

Vol 6 (S272) ◽

pp. 348-353 ◽

Cited By ~ 1

Author(s):

David H. Cohen ◽

Emma E. Wollman ◽

Maurice A. Leutenegger

Keyword(s):

Mass Loss ◽

Loss Rate ◽

Mass Loss Rate ◽

Broad Band ◽

Variable Structure ◽

Spectral Energy ◽

X Rays ◽

X Ray ◽

Spectral Diagnostics ◽

Loss Rates

AbstractX-rays give direct evidence of instabilities, time-variable structure, and shock heating in the winds of O stars. The observed broad X-ray emission lines provide information about the kinematics of shock-heated wind plasma, enabling us to test wind-shock models. And their shapes provide information about wind absorption, and thus about the wind mass-loss rates. Mass-loss rates determined from X-ray line profiles are not sensitive to density-squared clumping effects, and indicate mass-loss rate reductions of factors of 3 to 6 over traditional diagnostics that suffer from density-squared effects. Broad-band X-ray spectral energy distributions also provide mass-loss rate information via soft X-ray absorption signatures. In some cases, the degree of wind absorption is so high, that the hardening of the X-ray SED can be quite significant. We discuss these results as applied to the early O stars ζ Pup (O4 If), 9 Sgr (O4 V((f))), and HD 93129A (O2 If*).

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Five New Hot Jupiter Transits Investigated with Swift-UVOT

The Astronomical Journal ◽

10.3847/1538-3881/ac2c67 ◽

2021 ◽

Vol 162 (6) ◽

pp. 287

Author(s):

Lia Corrales ◽

Sasikrishna Ravi ◽

George W. King ◽

Erin May ◽

Emily Rauscher ◽

...

Keyword(s):

Mass Loss ◽

Loss Rate ◽

Mass Loss Rate ◽

Equilibrium Temperature ◽

Light Curves ◽

X Ray ◽

Hot Jupiters ◽

Upper Limits ◽

Marginal Detection ◽

Optical Radius

Abstract Short-wavelength exoplanet transit measurements have been used to probe mass loss in exoplanet atmospheres. We present the Swift-UVOT transit light curves for five hot Jupiters orbiting UV-bright F-type stars: XO-3, KELT-3, WASP-3, WASP-62, and HAT-P-6. We report one positive transit detection of XO-3b and one marginal detection of KELT-3b. We place upper limits on the remaining three transit depths. The planetary radii derived from the NUV transit depths of both potential detections are 50%–100% larger than their optical radius measurements. We examine the ratio R NUV/R opt for trends as a function of estimated mass-loss rate, which we derive from X-ray luminosity obtained from the Swift-XRT or, in the case of WASP-62, XMM-Newton. We find no correlation between the energy-limited photoevaporative mass-loss rate and the R NUV/R opt ratio. We also search for trends based on the equilibrium temperature of the hot Jupiters. We find a possible indication of a transition in the R NUV/R opt ratio around T eq = 1700 K, analogous to the trends found for NIR water features in transmission spectra. This might be explained by the formation of extended cloud decks with silicate particles ≤1 μm. We demonstrate that the Swift-UVOT filters could be sensitive to absorption from aerosols in exoplanet atmospheres.

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X-Ray Emission from Young Supernovae

Symposium - International Astronomical Union ◽

10.1017/s0074180900194240 ◽

2003 ◽

Vol 214 ◽

pp. 113-116

Author(s):

Stefan Immler

Keyword(s):

Mass Loss ◽

Loss Rate ◽

Mass Loss Rate ◽

Circumstellar Matter ◽

Physical Processes ◽

Reverse Shock ◽

X Ray

Observations of young SNe in the (∼ 0.1−100 keV) X-ray band allow to establish physical key parameters, such as the circumstellar matter (CSM) density, the mass-loss rate of the progenitor and the temperature of the outgoing and reverse shock as a function of time. Over the last ∼ 25 years, a small number of young SNe has been detected with orbiting X-ray observatories shortly after the outburst (days to months). Some highlights of recent observations with Chandra and XMM-Newton are presented and implications as to our understanding of the physical processes giving rise to the X-ray emission are briefly discussed.

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X-rays From Centrifugal Magnetospheres in Massive Stars

Proceedings of the International Astronomical Union ◽

10.1017/s1743921314007352 ◽

2014 ◽

Vol 9 (S307) ◽

pp. 449-450 ◽

Cited By ~ 1

Author(s):

Christopher Bard ◽

Richard Townsend

Keyword(s):

Mass Loss ◽

Loss Rate ◽

Massive Stars ◽

Mass Loss Rate ◽

X Rays ◽

Stellar Rotation ◽

Hydrodynamic Simulations ◽

X Ray ◽

Ob Stars ◽

Magnetically Confined

AbstractIn the subset of massive OB stars with strong global magnetic fields, X-rays arise from magnetically confined wind shocks (Babel & Montmerle 1997). However, it is not yet clear what the effect of stellar rotation and mass-loss rate is on these wind shocks and resulting X-rays. Here, we present results from a grid of Arbitrary Rigid-Field Hydrodynamic simulations (ARFHD) of a B-star centrifugal magnetosphere with an eye towards quantifying the effect of stellar rotation and mass-loss rate on the level of X-ray emission. The results are also compared to a generalized XADM model for X-rays in dynamical magnetospheres (ud-Doula et al. 2014).

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An X-ray study of mass-loss rate and wind acceleration of massive stars

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312013300 ◽

2011 ◽

Vol 7 (S279) ◽

pp. 351-352

Author(s):

Yoshitomo Maeda ◽

Yasuharu Sugawara ◽

Keyword(s):

Mass Loss ◽

Column Density ◽

Loss Rate ◽

Massive Stars ◽

Mass Loss Rate ◽

New Method ◽

Absorption Column ◽

X Ray ◽

Loss Rates

AbstractBy monitoring WC7 and the O5.5 binary WR 140 with the Suzaku telescope, we demonstrate a new method to measure the mass loss rates of both stars. By using the absorption column density, we found a mass-loss rate for the WC7 component: ṀWC7 ≈ 1.2 × 10−5 M⊙ yr−1. We also measured the mass-loss rate of the companion O component using a luminosity variation in phases: ṀO5.5 ≈ 5 × 10−7 M⊙ yr−1.

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