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  Astrophysical Parameters of LS 2883 and Implications for the PSR B1259-63 Gamma-ray Binary

Negueruela, I., Ribó, M., Herrero, A., Lorenzo, J., Khangulyan, D., & Aharonian, F. A. (2011). Astrophysical Parameters of LS 2883 and Implications for the PSR B1259-63 Gamma-ray Binary. Astrophysical Journal, Letters, 732(1): L11, pp. 1-5. doi:10.1088/2041-8205/732/1/L11.

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http://iopscience.iop.org/2041-8205/732/1 (Publisher version)
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Negueruela, Ignacio1, Author
Ribó, Marc2, Author
Herrero, Artemio3, 4, Author
Lorenzo, Javier1, Author
Khangulyan, Dmitry5, Author
Aharonian, Felix A.6, 7, Author           
Affiliations:
1Departamento de Fısica, Ingenierıa de Sistemas y Teorıa de la Senal, Universidad de Alicante, Apdo. 99, E-03080 Alicante, Spain, ou_persistent22              
2Departament d’Astronomia i Meteorologia, Institut de Ciences del Cosmos (ICC), Universitat de Barcelona (IEEC-UB), Martı i Franques 1, E-08028 Barcelona, Spain, ou_persistent22              
3Instituto de Astrof´ısica de Canarias, E-38200 La Laguna, Spain, ou_persistent22              
4Departamento de Astrofısica, Universidad de La Laguna, Avda. Astrofısico Francisco Sanchez, s/n, E-38205 La Laguna, Spain, ou_persistent22              
5Institute of Space and Astronautical Science/JAXA, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan, ou_persistent22              
6Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society, ou_904550              
7Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland, ou_persistent22              

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Free keywords: binaries: close – gamma rays: stars – pulsars: individual (PSR B1259–63) – stars: emission-line, Be – stars: individual (LS 2883) – X-rays: binaries
 Abstract: Only a few binary systems with compact objects display TeV emission. The physical properties of the companion stars represent basic input for understanding the physical mechanisms behind the particle acceleration, emission, and absorption processes in these so-called gamma-ray binaries. Here we present high-resolution and high signalto- noise optical spectra of LS 2883, the Be star forming a gamma-ray binary with the young non-accreting pulsar PSR B1259–63, showing it to rotate faster and be significantly earlier and more luminous than previously thought. Analysis of the interstellar lines suggests that the system is located at the same distance as (and thus is likely a member of) Cen OB1. Taking the distance to the association, d = 2.3 kpc, and a color excess of E(B −V ) = 0.85 for LS 2883 results in MV ≈ −4.4. Because of fast rotation, LS 2883 is oblate (Req 9.7 R and Rpole 8.1 R) and presents a temperature gradient (Teq ≈ 27,500 K, log geq = 3.7; Tpole ≈ 34,000 K, log gpole = 4.1). If the star did not rotate, it would have parameters corresponding to a late O-type star. We estimate its luminosity at log(L∗/L) 4.79 and its mass at M∗ ≈ 30 M. The mass function then implies an inclination of the binary system iorb ≈ 23◦, slightly smaller than previous estimates. We discuss the implications of these new astrophysical parameters of LS 2883 for the production of high-energy and very high-energy gamma rays in the PSR B1259–63/ LS 2883 gamma-ray binary system. In particular, the stellar properties are very important for prediction of the line-like bulk Comptonization component from the unshocked ultrarelativistic pulsar wind.

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 Dates: 2011-03-222011-04-08
 Publication Status: Issued
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 Identifiers: DOI: 10.1088/2041-8205/732/1/L11
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Title: Astrophysical Journal, Letters
  Other : ApJL
Source Genre: Journal
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Publ. Info: Chicago, IL : University of Chicago Press for the American Astronomical Society
Pages: 5 Volume / Issue: 732 (1) Sequence Number: L11 Start / End Page: 1 - 5 Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_1