Loading…
Nearly 30,000 late-type main-sequence stars with stellar age from LAMOST DR5
We construct a sample of nearly 30,000 main-sequence stars with 4500K \(
Saved in:
Published in: | arXiv.org 2020-11 |
---|---|
Main Authors: | , , , , , |
Format: | Article |
Language: | English |
Subjects: | |
Online Access: | Get full text |
Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
cited_by | |
---|---|
cites | |
container_end_page | |
container_issue | |
container_start_page | |
container_title | arXiv.org |
container_volume | |
creator | Zhang, Jiajun Zhao, Jingkun Oswalt, Terry D Liang, Xilong Ye, Xianhao Zhao, Gang |
description | We construct a sample of nearly 30,000 main-sequence stars with 4500K \( |
doi_str_mv | 10.48550/arxiv.2011.12477 |
format | article |
fullrecord | <record><control><sourceid>proquest</sourceid><recordid>TN_cdi_proquest_journals_2464483278</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2464483278</sourcerecordid><originalsourceid>FETCH-LOGICAL-a528-bd7e17e31d5f91534a99bedd4a8e5d0dbe9366d8a7d036a832dcd1fc3d275d333</originalsourceid><addsrcrecordid>eNotjl9LwzAUxYMgOOY-gG8BX21NcpMmfRzzz4TqQPs-bptb7ejamXTqvr0FfTqHA79zDmNXUqTaGSNuMfy0X6kSUqZSaWvP2EwByMRppS7YIsadEEJlVhkDM1a8EIbuxEHcTDHvcKRkPB2I77Htk0ifR-pr4nHEEPl3O35MlroOA8d34k0Y9rxYPm_eSn73ai7ZeYNdpMW_zln5cF-u1kmxeXxaLYsEjXJJ5S1JSyC9aXJpQGOeV-S9RkfGC19RDlnmHVovIEMHytdeNjV4ZY0HgDm7_qs9hGH6F8ftbjiGflrcKp1pPRHWwS8Z2k1V</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2464483278</pqid></control><display><type>article</type><title>Nearly 30,000 late-type main-sequence stars with stellar age from LAMOST DR5</title><source>Publicly Available Content Database</source><creator>Zhang, Jiajun ; Zhao, Jingkun ; Oswalt, Terry D ; Liang, Xilong ; Ye, Xianhao ; Zhao, Gang</creator><creatorcontrib>Zhang, Jiajun ; Zhao, Jingkun ; Oswalt, Terry D ; Liang, Xilong ; Ye, Xianhao ; Zhao, Gang</creatorcontrib><description>We construct a sample of nearly 30,000 main-sequence stars with 4500K \(<T\rm_{eff}<\) 5000K and stellar ages estimated by the chromospheric activity\(-\)age relation. This sample is used to determine the age distribution in the \(R-Z\) plane of the Galaxy, where \(R\) is the projected Galactocentric distance in the disk midplane and \(Z\) is the height above the disk midplane. As \(|Z|\) increases, the percentage of old stars becomes larger. It is known that scale-height of Galactic disk increases as \(R\) increases, which is called flare. A mild flare from \(R\) \(\sim\) 8.0 to 9.0 kpc in stellar age distribution is found. We also find that the velocity dispersion increases with age as confirmed by previous studies. Finally we present spiral-shaped structures in \(Z-\upsilon_{Z}\) phase space in three stellar age bins. The spiral is clearly seen in the age bin of [0, 1] Gyr, which suggests that a vertical perturbation to the disk probably took place within the last \(\sim\) 1.0 Gyr.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2011.12477</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Age ; Galactic disk ; Galaxy distribution ; Main sequence stars ; Perturbation ; Stellar age ; Stellar flares</subject><ispartof>arXiv.org, 2020-11</ispartof><rights>2020. This work is published under http://creativecommons.org/licenses/by-nc-sa/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktohtml>$$Uhttps://www.proquest.com/docview/2464483278?pq-origsite=primo$$EHTML$$P50$$Gproquest$$Hfree_for_read</linktohtml><link.rule.ids>776,780,25732,27904,36991,44569</link.rule.ids></links><search><creatorcontrib>Zhang, Jiajun</creatorcontrib><creatorcontrib>Zhao, Jingkun</creatorcontrib><creatorcontrib>Oswalt, Terry D</creatorcontrib><creatorcontrib>Liang, Xilong</creatorcontrib><creatorcontrib>Ye, Xianhao</creatorcontrib><creatorcontrib>Zhao, Gang</creatorcontrib><title>Nearly 30,000 late-type main-sequence stars with stellar age from LAMOST DR5</title><title>arXiv.org</title><description>We construct a sample of nearly 30,000 main-sequence stars with 4500K \(<T\rm_{eff}<\) 5000K and stellar ages estimated by the chromospheric activity\(-\)age relation. This sample is used to determine the age distribution in the \(R-Z\) plane of the Galaxy, where \(R\) is the projected Galactocentric distance in the disk midplane and \(Z\) is the height above the disk midplane. As \(|Z|\) increases, the percentage of old stars becomes larger. It is known that scale-height of Galactic disk increases as \(R\) increases, which is called flare. A mild flare from \(R\) \(\sim\) 8.0 to 9.0 kpc in stellar age distribution is found. We also find that the velocity dispersion increases with age as confirmed by previous studies. Finally we present spiral-shaped structures in \(Z-\upsilon_{Z}\) phase space in three stellar age bins. The spiral is clearly seen in the age bin of [0, 1] Gyr, which suggests that a vertical perturbation to the disk probably took place within the last \(\sim\) 1.0 Gyr.</description><subject>Age</subject><subject>Galactic disk</subject><subject>Galaxy distribution</subject><subject>Main sequence stars</subject><subject>Perturbation</subject><subject>Stellar age</subject><subject>Stellar flares</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><sourceid>PIMPY</sourceid><recordid>eNotjl9LwzAUxYMgOOY-gG8BX21NcpMmfRzzz4TqQPs-bptb7ejamXTqvr0FfTqHA79zDmNXUqTaGSNuMfy0X6kSUqZSaWvP2EwByMRppS7YIsadEEJlVhkDM1a8EIbuxEHcTDHvcKRkPB2I77Htk0ifR-pr4nHEEPl3O35MlroOA8d34k0Y9rxYPm_eSn73ai7ZeYNdpMW_zln5cF-u1kmxeXxaLYsEjXJJ5S1JSyC9aXJpQGOeV-S9RkfGC19RDlnmHVovIEMHytdeNjV4ZY0HgDm7_qs9hGH6F8ftbjiGflrcKp1pPRHWwS8Z2k1V</recordid><startdate>20201125</startdate><enddate>20201125</enddate><creator>Zhang, Jiajun</creator><creator>Zhao, Jingkun</creator><creator>Oswalt, Terry D</creator><creator>Liang, Xilong</creator><creator>Ye, Xianhao</creator><creator>Zhao, Gang</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope></search><sort><creationdate>20201125</creationdate><title>Nearly 30,000 late-type main-sequence stars with stellar age from LAMOST DR5</title><author>Zhang, Jiajun ; Zhao, Jingkun ; Oswalt, Terry D ; Liang, Xilong ; Ye, Xianhao ; Zhao, Gang</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a528-bd7e17e31d5f91534a99bedd4a8e5d0dbe9366d8a7d036a832dcd1fc3d275d333</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Age</topic><topic>Galactic disk</topic><topic>Galaxy distribution</topic><topic>Main sequence stars</topic><topic>Perturbation</topic><topic>Stellar age</topic><topic>Stellar flares</topic><toplevel>online_resources</toplevel><creatorcontrib>Zhang, Jiajun</creatorcontrib><creatorcontrib>Zhao, Jingkun</creatorcontrib><creatorcontrib>Oswalt, Terry D</creatorcontrib><creatorcontrib>Liang, Xilong</creatorcontrib><creatorcontrib>Ye, Xianhao</creatorcontrib><creatorcontrib>Zhao, Gang</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni)</collection><collection>ProQuest Central UK/Ireland</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>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering collection</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Zhang, Jiajun</au><au>Zhao, Jingkun</au><au>Oswalt, Terry D</au><au>Liang, Xilong</au><au>Ye, Xianhao</au><au>Zhao, Gang</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Nearly 30,000 late-type main-sequence stars with stellar age from LAMOST DR5</atitle><jtitle>arXiv.org</jtitle><date>2020-11-25</date><risdate>2020</risdate><eissn>2331-8422</eissn><abstract>We construct a sample of nearly 30,000 main-sequence stars with 4500K \(<T\rm_{eff}<\) 5000K and stellar ages estimated by the chromospheric activity\(-\)age relation. This sample is used to determine the age distribution in the \(R-Z\) plane of the Galaxy, where \(R\) is the projected Galactocentric distance in the disk midplane and \(Z\) is the height above the disk midplane. As \(|Z|\) increases, the percentage of old stars becomes larger. It is known that scale-height of Galactic disk increases as \(R\) increases, which is called flare. A mild flare from \(R\) \(\sim\) 8.0 to 9.0 kpc in stellar age distribution is found. We also find that the velocity dispersion increases with age as confirmed by previous studies. Finally we present spiral-shaped structures in \(Z-\upsilon_{Z}\) phase space in three stellar age bins. The spiral is clearly seen in the age bin of [0, 1] Gyr, which suggests that a vertical perturbation to the disk probably took place within the last \(\sim\) 1.0 Gyr.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2011.12477</doi><oa>free_for_read</oa></addata></record> |
fulltext | fulltext |
identifier | EISSN: 2331-8422 |
ispartof | arXiv.org, 2020-11 |
issn | 2331-8422 |
language | eng |
recordid | cdi_proquest_journals_2464483278 |
source | Publicly Available Content Database |
subjects | Age Galactic disk Galaxy distribution Main sequence stars Perturbation Stellar age Stellar flares |
title | Nearly 30,000 late-type main-sequence stars with stellar age from LAMOST DR5 |
url | http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-24T11%3A07%3A46IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Nearly%2030,000%20late-type%20main-sequence%20stars%20with%20stellar%20age%20from%20LAMOST%20DR5&rft.jtitle=arXiv.org&rft.au=Zhang,%20Jiajun&rft.date=2020-11-25&rft.eissn=2331-8422&rft_id=info:doi/10.48550/arxiv.2011.12477&rft_dat=%3Cproquest%3E2464483278%3C/proquest%3E%3Cgrp_id%3Ecdi_FETCH-LOGICAL-a528-bd7e17e31d5f91534a99bedd4a8e5d0dbe9366d8a7d036a832dcd1fc3d275d333%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_pqid=2464483278&rft_id=info:pmid/&rfr_iscdi=true |