DARTS/Astro Query System - SQL Search -
All the tables available for SQL Search and information on each table are listed in the Available Data page. Please see the User Guide for the usage of "SQL Search".
total 1
No. |
object_name
|
center_ra
|
center_dec
|
center_ra_b1950
|
center_dec_b1950
|
center_ecliptic_lon
|
center_ecliptic_lat
|
center_galactic_lon
|
center_galactic_lat
|
roll_angle
|
observation_start_time_mjd
|
observation_start_time
|
observation_end_time_mjd
|
observation_end_time
|
observation_id
|
exposure
|
awarded_exposure
|
xis0_exposure
|
xis1_exposure
|
xis2_exposure
|
xis3_exposure
|
xis0_observation_mode
|
xis1_observation_mode
|
xis2_observation_mode
|
xis3_observation_mode
|
hxd_observation_mode
|
hxd_coarse_clock_rate_exposure
|
hxd_first_clock_rate_exposure
|
hxd_normal_clock_rate_exposure
|
hxd_all_clock_rate_exposure
|
hxd_wam_exposure
|
quantity_of_hxd_burst
|
processing_status
|
processing_date_mjd
|
processing_date
|
public_date_mjd
|
public_date
|
distribution_date_mjd
|
distribution_date
|
processing_version
|
processing_count
|
processing_software
|
proposal_id
|
proposal_abstract
|
proposal_category
|
proposal_category_code
|
proposal_priority
|
pi_name
|
co_pi_name
|
proposal_affiliated_country
|
proposal_cycle
|
observation_type
|
proposal_title
|
main_instrument
|
has_xis_injection
|
data_access_url
|
ql_access_url
|
ql_image_url
|
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1 | V2301 OPH | 270.155 | 8.1565 | 269.554142 | 8.157196 | 270.169577 | 31.596745 | 34.53366867 | 14.97765204 | 262.0679 | 56576.0003009259 | 2013-10-11 00:00:26 | 56577.3452314815 | 2013-10-12 08:17:08 | 408024020 | 53.1884 | 110 | 53.1884 | 53.1884 | 0 | 53.1884 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.2892 | 47.2892 | 116.1898 | 0 | PROCESSED | 57612.9583333333 | 2016-08-12 23:00:00 | 57184 | 2015-06-11 00:00:00 | 56631.6754282407 | 2013-12-05 16:12:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080107 | It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion. | GALACTIC POINT SOURCES | 4 | A | TAKAYUKI HAYASHI | JAP | 8 | AO8 | MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408024020/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '408024020'
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