Active zone of the nucleus of the quasar 3C 273
The superfine structure of the quasar 3C 273 has been investigated at wavelengths λ = 2 and 6 cm with angular resolutions up to φ = 20 μ as for epochs 2005–2014. We have identified a nozzle and a bipolar outflow: a jet and a counterjet consisting of coaxial high- and low-velocity components. The sep...
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description | The superfine structure of the quasar 3C 273 has been investigated at wavelengths
λ
= 2 and 6 cm with angular resolutions up to
φ
= 20
μ
as for epochs 2005–2014. We have identified a nozzle and a bipolar outflow: a jet and a counterjet consisting of coaxial high- and low-velocity components. The separation between the nozzles in the plane of the sky is Δ
ρ
= 0.84 ± 0.16 pc; the flow ejection velocity is
v
≤ 0.1
c
. The nozzle brightness temperature reaches
T
b
≈ 45 × 10
12
K,
φ
= 20
μ
as,
λ
= 2 cm. The ejected electrons radiatively cool at a distance up to ≤4 pc. However, the jet afterglow is observed at a 8% level at a distance up to
ρ
≈ 16 pc; the acceleration compensates for the radiative losses. The reduction in the emission level of the central flow at large distances determines the jet bifurcation. The counterjet shape is a mirror reflection of the initial part of the jet, suggesting a symmetry and identity of the ejected flows. The counterjet and jet nozzles are in the near and remote parts of the active region, respectively. The emission from the nozzles is absorbed by a factor of 2 and 15, respectively. The absorption decreases with increasing distance and the brightness of the jet fragments rises to its maximum at 0.5 pc from the nozzle. Arclike structures, arm fragments, are observed in the region of the nozzles. The relativistic plasma comes to the nozzles and is ejected. The brightness temperature of the arclike structures reaches 10% of the peak value, which is determined by the a smaller optical depth, the visibility in the transverse direction. The central high-velocity flow is surrounded by low-velocity components, hollow tubes being ejected as an excess angular momentum is accumulated. The remainder of the material flows along the arms toward the disk center until the next accumulation of an excess angular momentum and the process is repeated. The diameter of the outer nozzle is Ø = 25 pc and, further out, decreases exponentially; Ø
n
≈ 80 exp(−1.15
n
) pc. The flow kinematics, collimation, and acceleration have a vortical nature. Ring currents producing magnetic fields, which accelerate and stabilize the processes, are generated in the rotating flows (tubes). The tangential directions of the currents are observed as parallel chains of components. |
doi_str_mv | 10.1134/S1063773717040053 |
format | Article |
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λ
= 2 and 6 cm with angular resolutions up to
φ
= 20
μ
as for epochs 2005–2014. We have identified a nozzle and a bipolar outflow: a jet and a counterjet consisting of coaxial high- and low-velocity components. The separation between the nozzles in the plane of the sky is Δ
ρ
= 0.84 ± 0.16 pc; the flow ejection velocity is
v
≤ 0.1
c
. The nozzle brightness temperature reaches
T
b
≈ 45 × 10
12
K,
φ
= 20
μ
as,
λ
= 2 cm. The ejected electrons radiatively cool at a distance up to ≤4 pc. However, the jet afterglow is observed at a 8% level at a distance up to
ρ
≈ 16 pc; the acceleration compensates for the radiative losses. The reduction in the emission level of the central flow at large distances determines the jet bifurcation. The counterjet shape is a mirror reflection of the initial part of the jet, suggesting a symmetry and identity of the ejected flows. The counterjet and jet nozzles are in the near and remote parts of the active region, respectively. The emission from the nozzles is absorbed by a factor of 2 and 15, respectively. The absorption decreases with increasing distance and the brightness of the jet fragments rises to its maximum at 0.5 pc from the nozzle. Arclike structures, arm fragments, are observed in the region of the nozzles. The relativistic plasma comes to the nozzles and is ejected. The brightness temperature of the arclike structures reaches 10% of the peak value, which is determined by the a smaller optical depth, the visibility in the transverse direction. The central high-velocity flow is surrounded by low-velocity components, hollow tubes being ejected as an excess angular momentum is accumulated. The remainder of the material flows along the arms toward the disk center until the next accumulation of an excess angular momentum and the process is repeated. The diameter of the outer nozzle is Ø = 25 pc and, further out, decreases exponentially; Ø
n
≈ 80 exp(−1.15
n
) pc. The flow kinematics, collimation, and acceleration have a vortical nature. Ring currents producing magnetic fields, which accelerate and stabilize the processes, are generated in the rotating flows (tubes). The tangential directions of the currents are observed as parallel chains of components.</description><identifier>ISSN: 1063-7737</identifier><identifier>EISSN: 1562-6873</identifier><identifier>DOI: 10.1134/S1063773717040053</identifier><language>eng</language><publisher>Moscow: Pleiades Publishing</publisher><subject>Acceleration ; Angular momentum ; Astronomy ; Astrophysics ; Astrophysics and Astroparticles ; Brightness temperature ; Ejection ; Emissions ; Flow velocity ; Fragments ; Kinematics ; Magnetic fields ; Nozzles ; Observations and Techniques ; Optical analysis ; Physics ; Physics and Astronomy ; Quasars ; Tubes ; Wavelengths</subject><ispartof>Astronomy letters, 2017-04, Vol.43 (4), p.221-232</ispartof><rights>Pleiades Publishing, Inc. 2017</rights><rights>Astronomy Letters is a copyright of Springer, 2017.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c334t-1c7536738a2409fe760cf986dc483e4ddb728e60abcc5ae9942d1ea45d42fece3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1134/S1063773717040053$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1134/S1063773717040053$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,776,780,27901,27902,41464,42533,51294</link.rule.ids></links><search><creatorcontrib>Matveyenko, L. I.</creatorcontrib><creatorcontrib>Seleznev, S. V.</creatorcontrib><title>Active zone of the nucleus of the quasar 3C 273</title><title>Astronomy letters</title><addtitle>Astron. Lett</addtitle><description>The superfine structure of the quasar 3C 273 has been investigated at wavelengths
λ
= 2 and 6 cm with angular resolutions up to
φ
= 20
μ
as for epochs 2005–2014. We have identified a nozzle and a bipolar outflow: a jet and a counterjet consisting of coaxial high- and low-velocity components. The separation between the nozzles in the plane of the sky is Δ
ρ
= 0.84 ± 0.16 pc; the flow ejection velocity is
v
≤ 0.1
c
. The nozzle brightness temperature reaches
T
b
≈ 45 × 10
12
K,
φ
= 20
μ
as,
λ
= 2 cm. The ejected electrons radiatively cool at a distance up to ≤4 pc. However, the jet afterglow is observed at a 8% level at a distance up to
ρ
≈ 16 pc; the acceleration compensates for the radiative losses. The reduction in the emission level of the central flow at large distances determines the jet bifurcation. The counterjet shape is a mirror reflection of the initial part of the jet, suggesting a symmetry and identity of the ejected flows. The counterjet and jet nozzles are in the near and remote parts of the active region, respectively. The emission from the nozzles is absorbed by a factor of 2 and 15, respectively. The absorption decreases with increasing distance and the brightness of the jet fragments rises to its maximum at 0.5 pc from the nozzle. Arclike structures, arm fragments, are observed in the region of the nozzles. The relativistic plasma comes to the nozzles and is ejected. The brightness temperature of the arclike structures reaches 10% of the peak value, which is determined by the a smaller optical depth, the visibility in the transverse direction. The central high-velocity flow is surrounded by low-velocity components, hollow tubes being ejected as an excess angular momentum is accumulated. The remainder of the material flows along the arms toward the disk center until the next accumulation of an excess angular momentum and the process is repeated. The diameter of the outer nozzle is Ø = 25 pc and, further out, decreases exponentially; Ø
n
≈ 80 exp(−1.15
n
) pc. The flow kinematics, collimation, and acceleration have a vortical nature. Ring currents producing magnetic fields, which accelerate and stabilize the processes, are generated in the rotating flows (tubes). The tangential directions of the currents are observed as parallel chains of components.</description><subject>Acceleration</subject><subject>Angular momentum</subject><subject>Astronomy</subject><subject>Astrophysics</subject><subject>Astrophysics and Astroparticles</subject><subject>Brightness temperature</subject><subject>Ejection</subject><subject>Emissions</subject><subject>Flow velocity</subject><subject>Fragments</subject><subject>Kinematics</subject><subject>Magnetic fields</subject><subject>Nozzles</subject><subject>Observations and Techniques</subject><subject>Optical analysis</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Quasars</subject><subject>Tubes</subject><subject>Wavelengths</subject><issn>1063-7737</issn><issn>1562-6873</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2017</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><recordid>eNqFkM1Lw0AQxRdRsFb_AG8BL15iZ3f2I3ssxS8QPKjnsN1MtCVN2t1E0L_eLVUQRTzNDO_3Hsxj7JTDBecoJw8cNBqDhhuQAAr32IgrLXJdGNxPe5LzrX7IjmJcAoBFhBGbTH2_eKXsvWsp6-qsf6GsHXxDQ_w6N4OLLmQ4y4TBY3ZQuybSyeccs6ery8fZTX53f307m97lHlH2OfdGoTZYOCHB1mQ0-NoWuvKyQJJVNTeiIA1u7r1yZK0UFScnVSVFTZ5wzM53uevQbQaKfblaRE9N41rqhlhyC1JwKRT-jxbWoOXAbULPfqDLbghtemRLpVJQqCJRfEf50MUYqC7XYbFy4a3kUG7bLn-1nTxi54mJbZ8pfEv-0_QBjAp8-Q</recordid><startdate>20170401</startdate><enddate>20170401</enddate><creator>Matveyenko, L. I.</creator><creator>Seleznev, S. V.</creator><general>Pleiades Publishing</general><general>Springer Nature B.V</general><scope>AAYXX</scope><scope>CITATION</scope><scope>3V.</scope><scope>7TG</scope><scope>7XB</scope><scope>88I</scope><scope>8FD</scope><scope>8FE</scope><scope>8FG</scope><scope>8FK</scope><scope>ABUWG</scope><scope>AEUYN</scope><scope>AFKRA</scope><scope>ARAPS</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>GNUQQ</scope><scope>H8D</scope><scope>HCIFZ</scope><scope>KL.</scope><scope>L7M</scope><scope>M2P</scope><scope>P5Z</scope><scope>P62</scope><scope>PHGZM</scope><scope>PHGZT</scope><scope>PKEHL</scope><scope>PQEST</scope><scope>PQGLB</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>Q9U</scope></search><sort><creationdate>20170401</creationdate><title>Active zone of the nucleus of the quasar 3C 273</title><author>Matveyenko, L. I. ; Seleznev, S. V.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c334t-1c7536738a2409fe760cf986dc483e4ddb728e60abcc5ae9942d1ea45d42fece3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2017</creationdate><topic>Acceleration</topic><topic>Angular momentum</topic><topic>Astronomy</topic><topic>Astrophysics</topic><topic>Astrophysics and Astroparticles</topic><topic>Brightness temperature</topic><topic>Ejection</topic><topic>Emissions</topic><topic>Flow velocity</topic><topic>Fragments</topic><topic>Kinematics</topic><topic>Magnetic fields</topic><topic>Nozzles</topic><topic>Observations and Techniques</topic><topic>Optical analysis</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>Quasars</topic><topic>Tubes</topic><topic>Wavelengths</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Matveyenko, L. I.</creatorcontrib><creatorcontrib>Seleznev, S. V.</creatorcontrib><collection>CrossRef</collection><collection>ProQuest Central (Corporate)</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>ProQuest Central (purchase pre-March 2016)</collection><collection>Science Database (Alumni Edition)</collection><collection>Technology Research Database</collection><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>ProQuest Central (Alumni) (purchase pre-March 2016)</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest One Sustainability</collection><collection>ProQuest Central UK/Ireland</collection><collection>Advanced Technologies & Aerospace Collection</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Science Database</collection><collection>Advanced Technologies & Aerospace Database</collection><collection>ProQuest Advanced Technologies & Aerospace Collection</collection><collection>ProQuest Central (New)</collection><collection>ProQuest One Academic (New)</collection><collection>ProQuest One Academic Middle East (New)</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Applied & Life Sciences</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central Basic</collection><jtitle>Astronomy letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Matveyenko, L. I.</au><au>Seleznev, S. V.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Active zone of the nucleus of the quasar 3C 273</atitle><jtitle>Astronomy letters</jtitle><stitle>Astron. Lett</stitle><date>2017-04-01</date><risdate>2017</risdate><volume>43</volume><issue>4</issue><spage>221</spage><epage>232</epage><pages>221-232</pages><issn>1063-7737</issn><eissn>1562-6873</eissn><abstract>The superfine structure of the quasar 3C 273 has been investigated at wavelengths
λ
= 2 and 6 cm with angular resolutions up to
φ
= 20
μ
as for epochs 2005–2014. We have identified a nozzle and a bipolar outflow: a jet and a counterjet consisting of coaxial high- and low-velocity components. The separation between the nozzles in the plane of the sky is Δ
ρ
= 0.84 ± 0.16 pc; the flow ejection velocity is
v
≤ 0.1
c
. The nozzle brightness temperature reaches
T
b
≈ 45 × 10
12
K,
φ
= 20
μ
as,
λ
= 2 cm. The ejected electrons radiatively cool at a distance up to ≤4 pc. However, the jet afterglow is observed at a 8% level at a distance up to
ρ
≈ 16 pc; the acceleration compensates for the radiative losses. The reduction in the emission level of the central flow at large distances determines the jet bifurcation. The counterjet shape is a mirror reflection of the initial part of the jet, suggesting a symmetry and identity of the ejected flows. The counterjet and jet nozzles are in the near and remote parts of the active region, respectively. The emission from the nozzles is absorbed by a factor of 2 and 15, respectively. The absorption decreases with increasing distance and the brightness of the jet fragments rises to its maximum at 0.5 pc from the nozzle. Arclike structures, arm fragments, are observed in the region of the nozzles. The relativistic plasma comes to the nozzles and is ejected. The brightness temperature of the arclike structures reaches 10% of the peak value, which is determined by the a smaller optical depth, the visibility in the transverse direction. The central high-velocity flow is surrounded by low-velocity components, hollow tubes being ejected as an excess angular momentum is accumulated. The remainder of the material flows along the arms toward the disk center until the next accumulation of an excess angular momentum and the process is repeated. The diameter of the outer nozzle is Ø = 25 pc and, further out, decreases exponentially; Ø
n
≈ 80 exp(−1.15
n
) pc. The flow kinematics, collimation, and acceleration have a vortical nature. Ring currents producing magnetic fields, which accelerate and stabilize the processes, are generated in the rotating flows (tubes). The tangential directions of the currents are observed as parallel chains of components.</abstract><cop>Moscow</cop><pub>Pleiades Publishing</pub><doi>10.1134/S1063773717040053</doi><tpages>12</tpages></addata></record> |
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subjects | Acceleration Angular momentum Astronomy Astrophysics Astrophysics and Astroparticles Brightness temperature Ejection Emissions Flow velocity Fragments Kinematics Magnetic fields Nozzles Observations and Techniques Optical analysis Physics Physics and Astronomy Quasars Tubes Wavelengths |
title | Active zone of the nucleus of the quasar 3C 273 |
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