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Journal articles on the topic 'Stars: individual: eta Carinae'

Author: Grafiati

Published: 4 June 2021

Last updated: 9 February 2022

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1

Groh, Jose H. "Zooming into Eta Carinae with interferometry." Proceedings of the International Astronomical Union 9, S307 (2014): 267–72. http://dx.doi.org/10.1017/s1743921314006917.

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AbstractShaped by strong mass loss, rapid rotation, and/or the presence of a close companion, the circumstellar environment around the most massive stars is complex and anything but spherical. Here we provide a brief overview of the high spatial resolution observations of Eta Carinae performed with the Very Large Telescope Interferometer (VLTI). Special emphasis is given to discuss VLTI/AMBER and VLTI/VINCI observations, which directly resolve spatial scales comparable to those where mass loss originates. Studying scales as small as a few milli-arcseconds allows us to investigate kinematical e

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2

Gull, Theodore R., and Augusto Damineli. "JD13 – Eta Carinae in the Context of the Most Massive Stars." Proceedings of the International Astronomical Union 5, H15 (2009): 373–98. http://dx.doi.org/10.1017/s1743921310009890.

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Eta Car, with its historical outbursts, visible ejecta and massive, variable winds, continues to challenge both observers and modelers. In just the past five years over 100 papers have been published on this fascinating object. We now know it to be a massive binary system with a 5.54-year period. In January 2009, η Car underwent one of its periodic low-states, associated with periastron passage of the two massive stars. This event was monitored by an intensive multi-wavelength campaign ranging from γ-rays to radio. A large amount of data was collected to test a number of evolving models includ

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3

Baratta, Giovanni Battista, and Roberto Viotti. "Eta Carinae: UV constraints on possible models. The close binary hypothesis." International Astronomical Union Colloquium 113 (1989): 277–78. http://dx.doi.org/10.1017/s0252921100004619.

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η Car is one of the brightest stars in our Galaxy. For its luminosity, huge mass loss, large variability can be considered as an ideal laboratory to study the LBV phenomenon, and to give constraints on possible models of LBVs. We propose that η Car is a – possibly binary –F-type hypergiantwhose wind isheated by dissipation of mechanical energy.

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Groh, J. H. "Multi-dimensional Modeling of Massive Binary Interaction in Eta Carinae." Proceedings of the International Astronomical Union 7, S282 (2011): 259–60. http://dx.doi.org/10.1017/s1743921311027505.

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AbstractWe summarize recent efforts from our group to constrain the nature of both stars in the Eta Carinae binary system and its orbital parameters by studying the influence of the companion star on the spectrum of the primary star. We find that the cavity in the dense wind of the primary star strongly affects multi-wavelength diagnostics such as the ultraviolet spectrum, the optical hydrogen lines, and the shape of the near-infrared continuum region. These diagnostics have been previously interpreted as requiring a latitude-dependent wind generated by a fast-rotating primary star, but the ef

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5

Kashi, Amit. "Accretion simulations of Eta Carinae and implications to massive binaries." Proceedings of the International Astronomical Union 14, S346 (2018): 93–97. http://dx.doi.org/10.1017/s1743921319002059.

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AbstractUsing high resolution 3D hydrodynamical simulations we quantify the amount of mass accreted onto the secondary star of the binary system η Carinae during periastron passage on its highly eccentric orbit. The accreted mass is responsible for the spectroscopic event occurring every orbit close to periastron passage, during which many lines vary and the x-ray emission associated with the destruction wind collision structure declines. The system is mainly known for its giant eruptions that occurred in the nineteenth century. The high mass model of the system, M1=170M⊙ and M2=80M⊙, gives Ma

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Viotti, R., L. Rossi, A. Altamore, C. Rossi, and A. Cassatella. "New Results on Eta Carinae. Evidence for an Asymmetric, Inhomogeneous Wind." Symposium - International Astronomical Union 116 (1986): 249–52. http://dx.doi.org/10.1017/s0074180900149022.

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The very peculiar object Eta Car is one of the best laboratory for the study of those physical processes - such as mass loss, superionization, dust condensation, wind interaction with the i.s. medium - that presently are of great astrophysical interest, especially for the study of the most luminous stars. For its light history and high luminosity Eta Car may also be considered as the galactic counterpart of the Hubble-Sandage variables. Eta Car is one of the rare astrophysical objects with evidence of dust condensation from ejected stellar matter (Andriesse et al. 78) On the other side the sta

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Dufour, Reginald J. "Oxygen Depletion Variations in Planetary Nebulae and Shells Ejected from Luminous Population I Stars." Symposium - International Astronomical Union 131 (1989): 216. http://dx.doi.org/10.1017/s0074180900138288.

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Recent studies by the Peimberts have noted an anticorrelation between 0 and N abundances in the Type I He- and N-rich PN, such that N+) is approximately constant. We report observations of the spectra and composition of several “planetary nebula-like” shells surrounding more luminous population I O- and WR-stars, which indicate that this 0-N anticorrelation extends upwards in the HR diagram to among the most luminous stars known, with O/H values in the shells ranging down to −2 dex below Solar. We report optical and UV spectrophotometry of the shell nebulae NGC 2359, NGC 6164-5, NGC 6888, NGC

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Massey, Philip, and Jennifer Johnson. "Massive stars near Eta Carinae - The stellar content of TR 14 and TR 16." Astronomical Journal 105 (March 1993): 980. http://dx.doi.org/10.1086/116487.

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9

Madura, Thomas I., Theodore Gull, Mairan Teodoro, et al. "4-D Imaging and Modeling of Eta Carinae’s Inner Fossil Wind Structures." Proceedings of the International Astronomical Union 12, S329 (2016): 420. http://dx.doi.org/10.1017/s1743921317000291.

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AbstractEta Carinae is the most massive active binary within 10,000 light-years and is famous for the largest non-terminal stellar explosion ever recorded. Observations reveal that the supermassive (~120 M⊙) binary, consisting of an LBV and either a WR or extreme O star, undergoes dramatic changes every 5.54 years due to the stars’ very eccentric orbits (e ≈ 0.9). Many of these changes are caused by a dynamic wind-wind collision region (WWCR) between the stars, plus expanding fossil WWCRs formed one, two, and three 5.54-year cycles ago. The fossil WWCRs can be spatially and spectrally resolved

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10

Madura, Thomas, T. R. Gull, N. Clementel, et al. "3D time-dependent hydrodynamical and radiative transfer modeling of Eta Carinae’s innermost fossil colliding wind structures." Proceedings of the International Astronomical Union 14, S346 (2018): 62–66. http://dx.doi.org/10.1017/s1743921318007949.

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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

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11

Smith, Nathan. "Eruptive outflow phases of massive stars." Proceedings of the International Astronomical Union 6, S272 (2010): 571–80. http://dx.doi.org/10.1017/s1743921311011458.

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AbstractI review recent progress on understanding eruptions of unstable massive stars, with particular attention to the diversity of observed behavior in extragalatic optical transient sources that are generally associated with giant eruptions of luminous blue variables (LBVs). These eruptions are thought to represent key mass loss episodes in the lives of massive stars. I discuss the possibility of dormant LBVs and implications for the duration of the greater LBV phase and its role in stellar evolution. These eruptive variables show a wide range of peak luminosity, decay time, expansion speed

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12

Damineli, A., M. Teodoro, N. D. Richardson, et al. "The wind-wind collision hole in eta Car." Proceedings of the International Astronomical Union 12, S329 (2016): 186–90. http://dx.doi.org/10.1017/s1743921317002630.

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AbstractEta Carinae is one of the most massive observable binaries. Yet determination of its orbital and physical parameters is hampered by obscuring winds. However the effects of the strong, colliding winds changes with phase due to the high orbital eccentricity. We wanted to improve measures of the orbital parameters and to determine the mechanisms that produce the relatively brief, phase-locked minimum as detected throughout the electromagnetic spectrum. We conducted intense monitoring of the He ii λ4686 line in η Carinae for 10 months in the year 2014, gathering ~300 high S/N spectra with

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13

Hyland, A. R., and G. Robinson. "Further Evidence for Large Grains in the Dust Shell Surrounding AG Carinae." Publications of the Astronomical Society of Australia 9, no. 1 (1991): 124–25. http://dx.doi.org/10.1017/s1323358000025170.

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AbstractThere is growing evidence for the notion that large grains are an important constituent of the interstellar medium. It has been found to be necessary to invoke the presence of large grains (of radius a > 1.0 μm) in a number of circumstellar shells, including those around Eta Carinae, and some late type giants and supergiants. Most recently, as a result of IRAS observations, the same idea has been used in the interpretation of the extensive optically thin disks found around some young early type stars. It is important to establish size constraints on these grains, so as to determine

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14

Wallerstein, George, and Kalpana K. Gilroy. "CCD observations of additional interstellar lines in stars associated with the VELA Remnant and Eta Carinae nebulosity." Astronomical Journal 103 (April 1992): 1346. http://dx.doi.org/10.1086/116148.

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15

Akashi, Muhammad, and Amit Kashi. "Fast ejecta resulted from jet–wind interaction in the Great Eruption of Eta Carinae." Monthly Notices of the Royal Astronomical Society 494, no. 3 (2020): 3186–99. http://dx.doi.org/10.1093/mnras/staa1014.

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ABSTRACT The accretion model for the 19th century Great Eruption (GE) of η Carinae suggests that mass outflowing from the primary was accreted on to the secondary, and the gravitational energy of that mass accounts for the increase in luminosity and most of the kinetic energy of the ejecta. It further argues that the accretion was accompanied by the ejection of two jets that shaped the bipolar Homunculus nebula. Observations of echos from the GE found emission lines with broad wings suggesting some of the mass in equatorial directions reached more than $10\, 000 \, \rm {km\, s^{-1}}$. We run h

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16

Gull, T. R., P. W. Morris, J. H. Black, et al. "Eta carinae and the homunculus: far infrared/submillimetre spectral lines detected with the Herschel Space Observatory." Monthly Notices of the Royal Astronomical Society 499, no. 4 (2020): 5269–301. http://dx.doi.org/10.1093/mnras/staa3113.

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ABSTRACT The evolved massive binary star η Carinae underwent eruptive mass-loss events that formed the complex bi-polar ‘Homunculus’ nebula harbouring tens of solar masses of unusually nitrogen-rich gas and dust. Despite expectations for the presence of a significant molecular component to the gas, detections have been observationally challenged by limited access to the far-infrared and the intense thermal continuum. A spectral survey of the atomic and rotational molecular transitions was carried out with the Herschel Space Observatory, revealing a rich spectrum of broad emission lines origina

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17

Owocki, Stanley P. "Continuum-driven versus line-driven mass loss and the Eddington limit." Proceedings of the International Astronomical Union 2, no. 14 (2006): 202–3. http://dx.doi.org/10.1017/s1743921307010150.

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AbstractBasic stellar structure dictates that stars of ∼ 100 M⊙ or more will be close to the Eddington limit, with luminosities in excess of 106 L⊙, and radiation pressure contributing prominently to the support against gravity. Although it is formally possible to generate static structure models of even more massive stars, recent studies of dense clusters show there is a sharp cutoff at masses above ∼ 150 M⊙. This talk examines the role of extreme mass loss is limiting the masses of stars, emphasizing in particular that continuum driving, possibly associated with structural instabilities of r

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18

Szécsényi-Nagy, G. "Data filtering in statistical studies of flares recorded in sky fields of stellar aggregates - demonstrated with the example of the Pleiades." Symposium - International Astronomical Union 137 (1990): 71–76. http://dx.doi.org/10.1017/s0074180900187479.

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Photometric data on flares of cluster flare stars published by different observers were - as a rule - collected during decades by different instruments and amidst various conditions. The uncritical use of these data in global statistical studies is usually unfair since such a collection is an indefinite mixture of high and low quality results. In order to make these investigations more reliable even the best and most complete photometric catalogues have to be filtered.The first step of the procedure described in the paper is rejecting all flare events having too small amplitudes - seeing that

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19

Weigelt, G., K. H. Hofmann, D. Schertl та ін. "VLTI-MATISSE chromatic aperture-synthesis imaging of η Carinae’s stellar wind across the Brα line". Astronomy & Astrophysics 652 (серпень 2021): A140. http://dx.doi.org/10.1051/0004-6361/202141240.

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Context. Eta Carinae is a highly eccentric, massive binary system (semimajor axis ~15.5 au) with powerful stellar winds and a phase-dependent wind-wind collision (WWC) zone. The primary star, η Car A, is a luminous blue variable (LBV); the secondary, η Car B, is a Wolf-Rayet or O star with a faster but less dense wind. Aperture-synthesis imaging allows us to study the mass loss from the enigmatic LBV η Car. Understanding LBVs is a crucial step toward improving our knowledge about massive stars and their evolution. Aims. Our aim is to study the intensity distribution and kinematics of η Car’s W

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