Standard

3C 345 : The variable component responsible for brightness increase of the object in the near-IR and optical regions in the early 1990's. / Hagen-Thorn, V. A.; Marchenko, S. G.; Takalo, L. O.; Sillanpää, A.

In: Astronomy and Astrophysics, Vol. 306, No. 1, 01.02.1996, p. 23-26.

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

Harvard

Hagen-Thorn, VA, Marchenko, SG, Takalo, LO & Sillanpää, A 1996, '3C 345: The variable component responsible for brightness increase of the object in the near-IR and optical regions in the early 1990's', Astronomy and Astrophysics, vol. 306, no. 1, pp. 23-26.

APA

Hagen-Thorn, V. A., Marchenko, S. G., Takalo, L. O., & Sillanpää, A. (1996). 3C 345: The variable component responsible for brightness increase of the object in the near-IR and optical regions in the early 1990's. Astronomy and Astrophysics, 306(1), 23-26.

Vancouver

Hagen-Thorn VA, Marchenko SG, Takalo LO, Sillanpää A. 3C 345: The variable component responsible for brightness increase of the object in the near-IR and optical regions in the early 1990's. Astronomy and Astrophysics. 1996 Feb 1;306(1):23-26.

Author

Hagen-Thorn, V. A. ; Marchenko, S. G. ; Takalo, L. O. ; Sillanpää, A. / 3C 345 : The variable component responsible for brightness increase of the object in the near-IR and optical regions in the early 1990's. In: Astronomy and Astrophysics. 1996 ; Vol. 306, No. 1. pp. 23-26.

BibTeX

@article{47bf6b6dedbf4253943ea47446eebf5e,
title = "3C 345: The variable component responsible for brightness increase of the object in the near-IR and optical regions in the early 1990's",
abstract = "An analysis of published data on variability of the blazar 3C 345 in the optical (B, V, R) and near-IR (J, H, K) regions in the 1991-92 brightness increase has been carried out. The relative spectral energy distribution of variable sources in both regions is shown to be unchanged irrespective of flux level. Combining these spectra to a single one shows that the same source is responsible for the variability in both regions. The combined spectrum is represented quite well by the spectrum of homogeneous synchrotron source. In the near-IR the observed spectra have the same slope as the spectrum of the variable source irrespective of flux level (i.e. the variable source is the main contributor to the observed flux even at the lowest flux level). In the optical region this is the case only for the spectra at high flux level. In minimum the contribution of the constant component is considerable. All these properties are the same as in the 1983-84 brightness increase of 3C 345 (see Paper I). The only difference is the spectral index of the variable source spectrum (in 1983-84 the spectrum was appreciably steeper).",
keywords = "Quasars: Individual: 3C 345, Radiation mechanisms: Non-thermal",
author = "Hagen-Thorn, {V. A.} and Marchenko, {S. G.} and Takalo, {L. O.} and A. Sillanp{\"a}{\"a}",
year = "1996",
month = feb,
day = "1",
language = "English",
volume = "306",
pages = "23--26",
journal = "ASTRONOMY & ASTROPHYSICS",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "1",

}

RIS

TY - JOUR

T1 - 3C 345

T2 - The variable component responsible for brightness increase of the object in the near-IR and optical regions in the early 1990's

AU - Hagen-Thorn, V. A.

AU - Marchenko, S. G.

AU - Takalo, L. O.

AU - Sillanpää, A.

PY - 1996/2/1

Y1 - 1996/2/1

N2 - An analysis of published data on variability of the blazar 3C 345 in the optical (B, V, R) and near-IR (J, H, K) regions in the 1991-92 brightness increase has been carried out. The relative spectral energy distribution of variable sources in both regions is shown to be unchanged irrespective of flux level. Combining these spectra to a single one shows that the same source is responsible for the variability in both regions. The combined spectrum is represented quite well by the spectrum of homogeneous synchrotron source. In the near-IR the observed spectra have the same slope as the spectrum of the variable source irrespective of flux level (i.e. the variable source is the main contributor to the observed flux even at the lowest flux level). In the optical region this is the case only for the spectra at high flux level. In minimum the contribution of the constant component is considerable. All these properties are the same as in the 1983-84 brightness increase of 3C 345 (see Paper I). The only difference is the spectral index of the variable source spectrum (in 1983-84 the spectrum was appreciably steeper).

AB - An analysis of published data on variability of the blazar 3C 345 in the optical (B, V, R) and near-IR (J, H, K) regions in the 1991-92 brightness increase has been carried out. The relative spectral energy distribution of variable sources in both regions is shown to be unchanged irrespective of flux level. Combining these spectra to a single one shows that the same source is responsible for the variability in both regions. The combined spectrum is represented quite well by the spectrum of homogeneous synchrotron source. In the near-IR the observed spectra have the same slope as the spectrum of the variable source irrespective of flux level (i.e. the variable source is the main contributor to the observed flux even at the lowest flux level). In the optical region this is the case only for the spectra at high flux level. In minimum the contribution of the constant component is considerable. All these properties are the same as in the 1983-84 brightness increase of 3C 345 (see Paper I). The only difference is the spectral index of the variable source spectrum (in 1983-84 the spectrum was appreciably steeper).

KW - Quasars: Individual: 3C 345

KW - Radiation mechanisms: Non-thermal

UR - http://www.scopus.com/inward/record.url?scp=0008991550&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:0008991550

VL - 306

SP - 23

EP - 26

JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

SN - 0004-6361

IS - 1

ER -

ID: 88369377