3D time-dependent hydrodynamical and radiative transfer modeling of Eta Carinae’s innermost fossil colliding wind structures

2018 ◽  
Vol 14 (S346) ◽  
pp. 62-66
Author(s):  
Thomas Madura ◽  
T. R. Gull ◽  
N. Clementel ◽  
M. Corcoran ◽  
A. Damineli ◽  
...  
Keyword(s):  
Radiative Transfer ◽  
Binary Systems ◽  
Hubble Space Telescope ◽  
Synthetic Data ◽  
Theoretical Models ◽  
Emission Lines ◽  
Time Dependent ◽  
Space Telescope ◽  
Data Cubes ◽  
Eta Carinae

AbstractEta Carinae is the most massive active binary within 10,000 light-years. While famous for the largest non-terminal stellar explosion ever recorded, observations reveal a supermassive (∼120 M⊙) binary consisting of an LBV and either a WR or extreme O star in a very eccentric orbit (e=0.9) with a 5.54-year period. Dramatic changes across multiple wavelengths are routinely observed as the stars move about in their highly elliptical orbits, especially around periastron when the hot (∼40 kK) companion star delves deep into the denser and much cooler (∼15 kK) extended wind photosphere of the LBV primary. Many of these changes are due to a dynamic wind-wind collision region (WWCR) that forms between the stars, plus expanding radiation-illuminated fossil WWCRs formed one, two, and three 5.54-year orbital cycles ago. These fossil WWCRs have been spatially and spectrally resolved by the Hubble Space Telescope/Space Telescope Imaging Spectrograph (HST/STIS) at multiple epochs, resulting in data cubes that spatially map Eta Carinae’s innermost WWCRs and follow temporal changes in several forbidden emission lines (e.g. [Fe iii] 4659 Å, [Fe ii] 4815 Å) across the 5.54-year cycle. We present initial results of 3D time-dependent hydrodynamical and radiative-transfer simulations of the Eta Carinae binary and its WWCRs with the goal of producing synthetic data cubes of forbidden emission lines for comparison to the available HST/STIS observations. Comparison of the theoretical models to the observations reveals important details about the binary’s orbital motion, photoionization properties, and recent (5–15year) mass loss history. Such an analysis also provides a baseline for following future changes in Eta Carinae, essential for understanding the late-stage evolution of a nearby supernova progenitor. Our modeling methods can also be adapted to a number of other colliding wind binary systems (e.g. WR 140) that are scheduled to be studied with future observatories (e.g. the James Webb Space Telescope).

scholarly journals UV Monochromatic Imaging of the Protoplanetary Nebula Hen 3-1475 Using HST STIS

Galaxies ◽  
2018 ◽  
Vol 6 (4) ◽  
pp. 141
Author(s):  
Xuan Fang ◽  
Martín Guerrero ◽  
Ana Castro ◽  
Jesús Toalá ◽  
Bruce Balick ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Critical Role ◽  
Planetary Nebulae ◽  
Emission Lines ◽  
Comparison Analysis ◽  
Space Telescope ◽  
Monochromatic Imaging ◽  
Protoplanetary Nebula ◽  
Low Dispersion ◽  
Negative Gradient

Collimated outflows and jets play a critical role in shaping planetary nebulae (PNe), especially in the brief transition from a spherical AGB envelope to an aspherical PN, which is called the protoplanetary nebula (pPN) phase. We present UV observations of Hen 3-1475, a bipolar pPN with fast, highly collimated jets, obtained with STIS on board the Hubble Space Telescope (HST). The deep, low-dispersion spectroscopy enabled monochromatic imaging of Hen 3-1475 in different UV nebular emission lines; this is the first of such attempt ever conducted for a pPN. The northwest inner knot (NW1) is resolved into four components in Mg ii λ 2800. Through comparison analysis with the HST optical narrowband images obtained 6 yr earlier, we found that these components of NW1 hardly move, despite of a negative gradient of high radial velocities, from −1550 km s - 1 on the innermost component to ∼−300 km s - 1 on the outermost. These NW1 knot components might thus be quasi-stationary shocks near the tip of the conical outflow of Hen 3-1475.

Astrometric Analysis of the Homunculus of eta Carinae With the Hubble Space Telescope

1996 ◽  
Vol 112 ◽  
pp. 1115 ◽  
Author(s):  
Douglas G. Currie ◽  
Daniel M. Dowling ◽  
Edward J. Shaya ◽  
Jeff Hester ◽  
Paul Scowen ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Space Telescope ◽  
Eta Carinae

Stellar Variability in the Central Populations of 47 Tucanae from WF/PC Observations with the Hubble Space Telescope. II. Binary Systems

1996 ◽  
Vol 468 ◽  
pp. 241 ◽  
Author(s):  
Peter D. Edmonds ◽  
Ronald L. Gilliland ◽  
Puragra Guhathakurta ◽  
Larry D. Petro ◽  
Abhijit Saha ◽  
...  
Keyword(s):  
Binary Systems ◽  
Hubble Space Telescope ◽  
Space Telescope

scholarly journals X-Ray Binaries in M51 I: Catalog and Statistics

2021 ◽  
Vol 922 (2) ◽  
pp. 178
Author(s):  
Jared R. Rice ◽  
Blagoy Rangelov ◽  
Andrea Prestwich ◽  
Rupali Chandar ◽  
Luis Bichon ◽  
...  
Keyword(s):  
Optical Properties ◽  
Data Analysis ◽  
Luminosity Function ◽  
Binary Systems ◽  
Hubble Space Telescope ◽  
Archival Data ◽  
Optical Counterpart ◽  
Space Telescope ◽  
X Ray ◽  
X Ray Binaries

Abstract We used archival data from the Chandra X-ray Observatory (Chandra) and the Hubble Space Telescope, to identify 334 candidate X-ray binary systems and their potential optical counterparts in the interacting galaxy pair NGC 5194/5195 (M51). We present the catalog and data analysis of X-ray and optical properties for those sources, from the deep 892 ks Chandra observations, along with the magnitudes of candidate optical sources as measured in the 8.16 ks Hubble Space Telescope observations. The X-ray luminosity function of the X-ray sources above a few times 1036 erg s−1 follows a power law N ( > L X , b ) ∝ L X , b 1 − α with α = 1.65 ± 0.03. Approximately 80% of sources are variable over a 30 day window. Nearly half of the X-ray sources (173/334) have an optical counterpart within 0.″5.

scholarly journals Deep [ITAL]Hubble Space Telescope[/ITAL] WFPC2 Photometry of NGC 288. I. Binary Systems and Blue Stragglers

2002 ◽  
Vol 123 (3) ◽  
pp. 1509-1527 ◽  
Author(s):  
Michele Bellazzini ◽  
Flavio Fusi Pecci ◽  
Maria Messineo ◽  
Lorenzo Monaco ◽  
Robert T. Rood
Keyword(s):  
Binary Systems ◽  
Hubble Space Telescope ◽  
Space Telescope ◽  
Blue Stragglers

Imaging polarimetry of eta carinae with the hubble space telescope

1999 ◽  
pp. 255-259
Author(s):  
Regina E. Schulte-Ladbeck ◽  
Anna Pasquali ◽  
Mark Clampin ◽  
Antonella Nota ◽  
John Hillier ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Space Telescope ◽  
Eta Carinae ◽  
Imaging Polarimetry

scholarly journals Galaxies with Binary Nuclei

2013 ◽  
Vol 9 (S304) ◽  
pp. 363-370
Author(s):  
Yervant Terzian ◽  
Edward Khachikian
Keyword(s):  
Hubble Space Telescope ◽  
Radio Galaxies ◽  
Active Galaxies ◽  
Emission Lines ◽  
Special Astrophysical Observatory ◽  
Host Galaxies ◽  
Strong Emission ◽  
Space Telescope ◽  
Byurakan Astrophysical Observatory ◽  
The Common

AbstractIt is known that among active galaxies (AG) with strong emission lines (UV-galaxies, Sy1 and Sy2, Markarian and Kazarian galaxies, radio-galaxies, QSOs host galaxies and so on) there is a large percentage of objects with double and multiple (or complex) nuclei. The common sizes of these nuclei are of the order of a few hundred parsecs or kiloparsecs. We shall discuss the results of morphological and spectroscopic observations of a number of “active galaxies” carried out with the 5m Palomar telescope, 2.6m telescope of Ambartsumian Byurakan Astrophysical Observatory, 6m telescope of Special Astrophysical Observatory in Russia, and newer Hubble Space Telescope data.

scholarly journals Inflowing gas in the central parsec of M81

2019 ◽  
Vol 488 (1) ◽  
pp. 1199-1210 ◽  
Author(s):  
Nick Devereux
Keyword(s):  
Hubble Space Telescope ◽  
Line Emission ◽  
Visible Spectrum ◽  
Emission Lines ◽  
Extended Source ◽  
Space Telescope ◽  
X Ray ◽  
Wide Range ◽  
Low Metallicity ◽  
Central Parsec

Abstract Spectroscopic observations of the Seyfert 1/Liner nucleus of M81, obtained recently with the Space Telescope Imaging Spectrograph aboard the Hubble Space Telescope(HST), have revealed an ultraviolet (UV)–visible spectrum rich with emission lines of a variety of widths, ionization potentials, and critical densities, including several in the UV that have not previously been reported. Even at the highest angular resolution currently achievable with HST, the broad-line region of M81 cannot be uniquely defined on the basis of commonly used observables such as the full width at half-maximum of the emission lines, or ratios of various emission lines. Numerous broad forbidden lines complicate interpretation of the spectra. At least three separate line-emitting components are inferred. Firstly, a large, highly ionized, low-density, low-metallicity H+ region producing the broad Balmer lines. Located within the H+ region are smaller condensations spanning a wide range in density, and the source of forbidden line emission through collisional excitation of the respective ions. Intermingled with the H+ region and the condensations is a curious extended source of time-variable C iv λ1548 emission. Collectively, these observations can be qualitatively understood in the context of a shock-excited jet cavity within a large H+ region that is photoionized by the central UV–X-ray source. The H+ region contains ∼500 M⊙ of low-metallicity gas that is dynamically unstable to inflow. At the current rate, the available H+ gas can sustain the advection-dominated accretion flow that powers the central UV–X-ray source for 105 yr.

scholarly journals Eta Carinae: A Tale of Two Periastron Passages

2021 ◽  
Vol 923 (1) ◽  
pp. 102
Author(s):  
Theodore R. Gull ◽  
Felipe Navarete ◽  
Michael F. Corcoran ◽  
Augusto Damineli ◽  
David Espinoza ◽  
...  
Keyword(s):  
Transient Absorption ◽  
Hubble Space Telescope ◽  
Wavelength Dependence ◽  
Primary Star ◽  
Space Telescope ◽  
Eta Carinae ◽  
Secondary Star ◽  
Order Of Magnitude ◽  
Far Ultraviolet ◽  
First Time

Abstract Since 2002, the far-ultraviolet (FUV) flux (1150–1680 Å) of Eta Carinae, monitored by the Hubble Space Telescope/Space Telescope Imaging Spectrograph, has increased by an order of magnitude. This increase is attributed to partial dissipation of a line-of-sight (LOS) occulter that blocks the central core of the system. Across the 2020 February periastron passage, changes in the FUV emission show a stronger wavelength dependence than occurred across the 2003 July periastron passage. Across both periastron passages, most of the FUV spectrum dropped in flux then recovered a few months later. The 2020 periastron passage included enhancements of FUV flux in narrow spectral intervals near periastron followed by a transient absorption and recovery to pre-periastron flux levels. The drop in flux is due to increased absorption by singly ionized species as the secondary star plunges deep into the wind of the primary star, which blocks the companion’s ionizing radiation. The enhanced FUV emission is caused by the companion’s wind-blown cavity briefly opening a window to deeper layers of the primary star. This is the first time transient brightening has been seen in the FUV comparable to transients previously seen at longer wavelengths. Changes in resonance line-velocity profiles hint that the dissipating occulter is associated with material in LOS moving at −100 to −300 km s−1, similar in velocity of structures previously associated with the 1890s lesser eruption.

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