X-ray spectroscopy of massive stellar winds: previous and ongoing observations of the hot star ζ Pup

N. Miller; W. Waldron; J. Nichols; D. Huenemoerder; M. Dahmer; R. Ignace; J. Lauer; A. Moffat; Y. Nazé; L. Oskinova; N. Richardson; T. Ramiaramanantsoa; T. Shenar; K. Gayley

doi:10.1017/S1743921319001340

X-ray spectroscopy of massive stellar winds: previous and ongoing observations of the hot star ζ Pup

N. Miller, W. Waldron, J. Nichols, D. Huenemoerder, M. Dahmer, R. Ignace, J. Lauer, A. Moffat, Y. Nazé, L. Oskinova, N. Richardson, T. Ramiaramanantsoa, T. Shenar, K. Gayley

Research output: Contribution to journal › Article › peer-review

Abstract

The stellar winds of hot stars have an important impact on both stellar and galactic evolution, yet their structure and internal processes are not fully understood in detail. One of the best nearby laboratories for studying such massive stellar winds is the O4I(n)fp star ζ Pup. After briefly discussing existing X-ray observations from Chandra and XMM, we present a simulation of X-ray emission line profile measurements for the upcoming 840 kilosecond Chandra HETGS observation. This simulation indicates that the increased S/N of this new observation will allow several major steps forward in the understanding of massive stellar winds. By measuring X-ray emission line strengths and profiles, we should be able to differentiate between various stellar wind models and map the entire wind structure in temperature and density. This legacy X-ray spectrum of ζ Pup will be a useful benchmark for future X-ray missions.

Original language	English
Pages (from-to)	88-92
Number of pages	5
Journal	Proceedings of the International Astronomical Union
Volume	14
DOIs	https://doi.org/10.1017/S1743921319001340
State	Published - 1 Aug 2018
Externally published	Yes

Keywords

X-rays: stars
outflows
stars: early-type
stars: mass loss
stars: winds

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1017/S1743921319001340

Cite this

Miller, N., Waldron, W., Nichols, J., Huenemoerder, D., Dahmer, M., Ignace, R., Lauer, J., Moffat, A., Nazé, Y., Oskinova, L., Richardson, N., Ramiaramanantsoa, T., Shenar, T., & Gayley, K. (2018). X-ray spectroscopy of massive stellar winds: previous and ongoing observations of the hot star ζ Pup. Proceedings of the International Astronomical Union, 14, 88-92. https://doi.org/10.1017/S1743921319001340

@article{09529284a6d7433b96c3970f354ab2eb,

title = "X-ray spectroscopy of massive stellar winds: previous and ongoing observations of the hot star ζ Pup",

abstract = "The stellar winds of hot stars have an important impact on both stellar and galactic evolution, yet their structure and internal processes are not fully understood in detail. One of the best nearby laboratories for studying such massive stellar winds is the O4I(n)fp star ζ Pup. After briefly discussing existing X-ray observations from Chandra and XMM, we present a simulation of X-ray emission line profile measurements for the upcoming 840 kilosecond Chandra HETGS observation. This simulation indicates that the increased S/N of this new observation will allow several major steps forward in the understanding of massive stellar winds. By measuring X-ray emission line strengths and profiles, we should be able to differentiate between various stellar wind models and map the entire wind structure in temperature and density. This legacy X-ray spectrum of ζ Pup will be a useful benchmark for future X-ray missions.",

keywords = "X-rays: stars, outflows, stars: early-type, stars: mass loss, stars: winds",

author = "N. Miller and W. Waldron and J. Nichols and D. Huenemoerder and M. Dahmer and R. Ignace and J. Lauer and A. Moffat and Y. Naz{\'e} and L. Oskinova and N. Richardson and T. Ramiaramanantsoa and T. Shenar and K. Gayley",

note = "Publisher Copyright: {\textcopyright} International Astronomical Union 2019.",

year = "2018",

month = aug,

day = "1",

doi = "10.1017/S1743921319001340",

language = "الإنجليزيّة",

volume = "14",

pages = "88--92",

journal = "Proceedings of the International Astronomical Union",

issn = "1743-9213",

publisher = "Cambridge University Press",

}

Miller, N, Waldron, W, Nichols, J, Huenemoerder, D, Dahmer, M, Ignace, R, Lauer, J, Moffat, A, Nazé, Y, Oskinova, L, Richardson, N, Ramiaramanantsoa, T, Shenar, T & Gayley, K 2018, 'X-ray spectroscopy of massive stellar winds: previous and ongoing observations of the hot star ζ Pup', Proceedings of the International Astronomical Union, vol. 14, pp. 88-92. https://doi.org/10.1017/S1743921319001340

TY - JOUR

T1 - X-ray spectroscopy of massive stellar winds

T2 - previous and ongoing observations of the hot star ζ Pup

AU - Miller, N.

AU - Waldron, W.

AU - Nichols, J.

AU - Huenemoerder, D.

AU - Dahmer, M.

AU - Ignace, R.

AU - Lauer, J.

AU - Moffat, A.

AU - Nazé, Y.

AU - Oskinova, L.

AU - Richardson, N.

AU - Ramiaramanantsoa, T.

AU - Shenar, T.

AU - Gayley, K.

PY - 2018/8/1

Y1 - 2018/8/1

N2 - The stellar winds of hot stars have an important impact on both stellar and galactic evolution, yet their structure and internal processes are not fully understood in detail. One of the best nearby laboratories for studying such massive stellar winds is the O4I(n)fp star ζ Pup. After briefly discussing existing X-ray observations from Chandra and XMM, we present a simulation of X-ray emission line profile measurements for the upcoming 840 kilosecond Chandra HETGS observation. This simulation indicates that the increased S/N of this new observation will allow several major steps forward in the understanding of massive stellar winds. By measuring X-ray emission line strengths and profiles, we should be able to differentiate between various stellar wind models and map the entire wind structure in temperature and density. This legacy X-ray spectrum of ζ Pup will be a useful benchmark for future X-ray missions.

AB - The stellar winds of hot stars have an important impact on both stellar and galactic evolution, yet their structure and internal processes are not fully understood in detail. One of the best nearby laboratories for studying such massive stellar winds is the O4I(n)fp star ζ Pup. After briefly discussing existing X-ray observations from Chandra and XMM, we present a simulation of X-ray emission line profile measurements for the upcoming 840 kilosecond Chandra HETGS observation. This simulation indicates that the increased S/N of this new observation will allow several major steps forward in the understanding of massive stellar winds. By measuring X-ray emission line strengths and profiles, we should be able to differentiate between various stellar wind models and map the entire wind structure in temperature and density. This legacy X-ray spectrum of ζ Pup will be a useful benchmark for future X-ray missions.

KW - X-rays: stars

KW - outflows

KW - stars: early-type

KW - stars: mass loss

KW - stars: winds

UR - http://www.scopus.com/inward/record.url?scp=85077467499&partnerID=8YFLogxK

U2 - 10.1017/S1743921319001340

DO - 10.1017/S1743921319001340

M3 - مقالة

SN - 1743-9213

VL - 14

SP - 88

EP - 92

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

ER -

X-ray spectroscopy of massive stellar winds: previous and ongoing observations of the hot star ζ Pup

Abstract

Keywords

All Science Journal Classification (ASJC) codes

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