A method and system for generating real-time pulsar time independent of atomic time systems

Abstract

The application discloses a kind of independent atomic time system real-time pulsar time generation method and system, the method comprises the following steps: S1.select N radio pulsars, observation and record observation data;S2.pulse arrival time is obtained;S3.traces to international atomic time;S4.international atomic time time corresponding pulse arrival time and time residual error are calculated;S5.determine the longest time scale corresponding to the red noise that can be fitted by second-order polynomial;S6.pulsar observation time corresponding to the discrete pulsar time is calculated;S7.any time observation station atomic clock time scale corresponding real-time pulsar time is obtained;S8.with the same observation interval and data recording mode, N pulsars are successively observed, and the real-time pulsar time generated in S7 is used to replace international atomic time to calculate pulse arrival time residual error;S9.using the data of the last 4 years of the pulsar, repeat step S5;S10.real-time pulsar time is obtained;S11.S8-S10 is repeated, and real-time pulsar time is obtained.

Description

Technical Field

[0001] This invention relates to the fields of astronomy and computer communication, specifically to a real-time pulsar time generation method and system that utilizes multiple pulsars for radio observations independent of atomic time systems. Background Technology

[0002] Currently, there are technologies that utilize pulsar observations to generate non-real-time pulsar times corresponding to past atomic times to correct atomic times or verify the stability of atomic times. The current method involves observing pulsars with known rotational patterns, determining the pulsar pulse arrival time using the atomic clock reading at the observatory, assuming the difference between the non-real-time pulsar time and the atomic time is a piecewise polynomial function, or assuming this difference has a power-law spectrum, and then directly using the least squares method or Bayesian methods to fit the corresponding polynomial function or spectral parameters with the pulse arrival time to obtain the corresponding function for the non-real-time pulsar time.

[0003] The methods described above can only provide non-real-time pulsar times within the time period corresponding to the telescope observation of the pulsar, not real-time pulsar times. Therefore, these methods can only be used to verify past times, not for timing. Furthermore, these methods require continuous comparison of the pulse arrival time with International Atomic Time (IAT). If the pulsar observation deviates from IAT, these non-real-time pulsar time generation methods cannot be used. Summary of the Invention

[0004] To address the problems existing in the prior art, the purpose of this invention is to provide a method and system for generating real-time pulsar time independent of the atomic time system using radio observations of multiple pulsars. This method can generate real-time pulsar time, and when performing real-time timing, it is not necessary to compare the arrival time of the pulsar pulse with International Atomic Time.

[0005] To achieve the above objectives, the present invention provides a real-time pulsar time generation method independent of atomic time systems, the method comprising the following steps:

[0006] S1. Select N radio pulsars with known rotation patterns, and use a radio telescope to successively observe and record the observation data of the N pulsars. Continue the observation for the first stage. The total number of observations of the nth pulsar is denoted as I. n ;

[0007] S2. Process the obtained pulsar observation data to obtain the pulsar pulse arrival time T. ni , where the subscript n represents the nth pulsar and the subscript i represents the i-th observation;

[0008] S3. The obtained pulse arrival time T ni Tracing back to International Atomic Time T′ ni;

[0009] S4. Calculate the international atomic time T′ based on the known rotation laws of pulsars. ni The pulse arrival time T″ corresponding to the moment ni and pulse arrival time residual δT ni =T″ ni -T′ ni ;

[0010] S5. Analyze δT of each pulsar ni The power spectrum was used to determine the pulse arrival time residual δT for each pulsar. ni The power spectrum can be fitted with a second-order polynomial to the longest timescale δt corresponding to the red noise. n ;

[0011] S6. Use the δt obtained from the analysis in step S5. n The pulsar observation time T is obtained by calculation with a second-order polynomial. ni The corresponding discrete pulsar time t p (T ni );

[0012] S7. Using pulsar observations to determine the atomic clock reading T at the observation station ni t p (T ni The discrete pulsar time corresponds to the real-time pulsar time t corresponding to the atomic clock reading T at any given moment at the observation station. p (T);

[0013] S8. After the pulsar observation in S1, observe N pulsars successively with the same observation interval and data recording method, record the observation data, and process the data using the steps in S2 to obtain the pulse arrival time. Use the real-time pulsar time generated in S7 to replace the international atomic time to calculate the pulse arrival time residual.

[0014] S9. After each pulsar data update, repeat the processing in step S5 using the data from the most recent 4 years of this pulsar to obtain the second-order polynomial corresponding to the pulsar and the longest timescale corresponding to the fitted red noise.

[0015] S10. Using the parameters obtained in S8 and S9, the real-time pulsar time is obtained using the methods in S6 and S7;

[0016] S11. After each new pulsar observation, execute S8-S10 again to obtain the real-time pulsar time corresponding to the atomic clock reading at the observatory after the latest observation.

[0017] Furthermore, N is greater than or equal to 10.

[0018] Furthermore, in step S1, the first phase lasts for 4 years; the observation time for each pulsar is no less than 15 minutes, and the interval between two consecutive observations of each pulsar is maintained between 10 and 20 days.

[0019] Furthermore, in step S1, the observation data includes the variation of radiation data of different frequencies of pulsar radiation over time and the observation time.

[0020] Furthermore, in step S2, the pulse arrival time obtained is based on the atomic clock reading at the observation station.

[0021] Furthermore, in step S3, during the process of tracing back to International Atomic Time, tracing the atomic clock readings of the observation station to International Atomic Time requires the use of clock difference files obtained through satellite navigation systems that are compared with Standard Coordinated Universal Time, as well as time difference files between different times provided by the International Earth Rotation and Reference Systems Service.

[0022] Furthermore, in step S4, after obtaining the pulse arrival time residual δT ni At the same time, the error of the pulse arrival time residual can be obtained.

[0023] Furthermore, in step S5, the power spectrum of the pulsar pulse arrival time residual... The superposition of red noise with a power-law spectrum and white noise with a flat spectrum is used, and the power spectrum of the pulsar pulse arrival time residual is set to be equal to a power-law function. With a constant function S n1 (t)=C n The sum of these parameters is used to fit the power spectrum of the observed pulsar pulse arrival time residuals to obtain the parameters k of the power-law function and the constant function. n α n With C n ; in the pulse arrival time residual sequence δT corresponding to the same index n ni In, there exists δt n1 Makes any sequence and The correspondence is achieved using the second-order polynomial δT ni =aT′ ni 2 +bT′ ni After fitting with +c, the standard deviation of the corresponding fitting residuals is... All less than or equal to δt that satisfies the above conditions n1 In the middle, the largest one is denoted as δt. n The longest timescale corresponding to the red noise is fitted using a second-order polynomial.

[0024] Furthermore, in step S6, during each pulsar observation T... ni When, select the nth k Distance T of pulsar ni Time length less than Pulse arrival time residuals obtained from observation data processing Extrapolate using the polynomial obtained in step S5 to predict T. ni Pulse arrival time residual corresponding to time 1 by As weight pairs Perform a weighted average to obtain the pulsar observation time T. ni The corresponding discrete pulsar time t p (T ni ).

[0025] On the other hand, the present invention provides a real-time pulsar time generation system independent of atomic time system. The system is used to implement the real-time pulsar time generation method independent of atomic time system according to the present invention. The system includes an observation module and a calculation module. The observation module is used to observe N pulsars to obtain observation data, and the calculation module is used to generate real-time pulsar time based on the observation data and the local clock reading of the observation station.

[0026] Beneficial effects:

[0027] This invention eliminates the influence of pulsar timing red noise through a polynomial fitting process within a short timescale, resulting in real-time pulsar times with higher frequency stability.

[0028] After the invention begins generating real-time pulsar times, it will operate independently of the atomic time system and generate real-time pulsar times.

[0029] This invention can obtain real-time pulsar times without complex data processing. Attached Figure Description

[0030] Figure 1 This is an overall flowchart of the real-time pulsar time generation method of the present invention, which is independent of the atomic time system;

[0031] Figure 2 In a specific embodiment of the present invention, the deviation between the real-time pulsar time generated by the method of generating real-time pulsar time independent of the atomic time system using radio observations of multiple pulsars in the present invention based on simulation data and International Atomic Time is described. Detailed Implementation

[0032] The technical solution of the present invention will now be clearly and completely described with reference to the accompanying drawings. Obviously, the described embodiments are only some, not all, of the embodiments of the present invention. Based on the embodiments of the present invention, all other embodiments obtained by those skilled in the art without creative effort are within the scope of protection of the present invention.

[0033] In the description of this invention, it should be noted that the terms "center," "upper," "lower," "left," "right," "vertical," "horizontal," "inner," and "outer," etc., indicate the orientation or positional relationship based on the orientation or positional relationship shown in the accompanying drawings. They are used only for the convenience of describing the invention and for simplifying the description, and do not indicate or imply that the device or element referred to must have a specific orientation, or be constructed and operated in a specific orientation. Therefore, they should not be construed as limitations on the invention. Furthermore, the terms "first," "second," and "third" are used for descriptive purposes only and should not be construed as indicating or implying relative importance.

[0034] In the description of this invention, it should be noted that, unless otherwise explicitly specified and limited, the terms "installation," "connection," and "linking" should be interpreted broadly. For example, they can refer to a fixed connection, a detachable connection, or an integral connection; they can refer to a mechanical connection or an electrical connection; they can refer to a direct connection or an indirect connection through an intermediate medium; and they can refer to the internal connection of two components. Those skilled in the art can understand the specific meaning of the above terms in this invention according to the specific circumstances.

[0035] The following combination Figures 1-2 Specific embodiments of the present invention will be described in detail below. It should be understood that the specific embodiments described herein are for illustrative and explanatory purposes only and are not intended to limit the present invention.

[0036] This invention provides a method for generating real-time pulsar time independent of the atomic time system using radio observations of multiple pulsars. The basic concept is to generate real-time pulsar time independent of the atomic time system based on radio observations of multiple pulsars. The pulsar radio observation process requires the observation and recording of radio pulsar signals using a radio telescope and its back-end equipment. The atomic time system is a time system obtained by weighted averaging of the readings of multiple atomic clocks and using a frequency standard clock as the driving force; International Atomic Time (IAT) belongs to the atomic time system. Pulsar time is defined based on the rotational stability of pulsars. Real-time pulsar time is defined as pulsar time that can be generated in real time; conversely, non-real-time pulsar time is defined as pulsar time corresponding only to a past period. Specifically, the discrete pulsar time mentioned in this example is defined as the pulsar time corresponding to certain discrete moments. The atomic clock reading at the observatory refers to the time displayed in real time using the atomic clock located at the observatory, which has a certain deviation from IAT.

[0037] This invention provides a method for generating real-time pulsar times independent of atomic-time systems based on radio observations of multiple pulsars, such as... Figure 1 As shown, the method includes the following steps:

[0038] S1. Select N radio pulsars with known rotation patterns, and use a radio telescope to successively observe and record the observation data of the N pulsars. Continue the observation for the first stage. The total number of observations of the nth pulsar is denoted as I. n To obtain pulsar observation data. Preferably, N is greater than or equal to 10, and the first phase lasts for 4 years.

[0039] Currently, publicly available pulsar rotation parameters can be found on relevant websites, and known pulsar spin-jump events can also be obtained from relevant web pages. This first phase of observation involves selecting more than 10 radio pulsars with known rotation patterns, a flux of over 0.05 mJy at 1400 MHz, and no known spin-jump events. These pulsars will be observed sequentially using radio telescopes, and the observation data will be recorded. This first phase of observation will last for 4 years. Each observation of each pulsar should last more than 15 minutes to obtain a stable average pulse profile. The interval between two consecutive observations of each pulsar should be 10-20 days. The total number of observations of the nth pulsar in the first phase is denoted as I. n In step S1, the data is recorded in the standard pulsar data format PSRFITS, which records the pulsar observation time, the pulsar flux at each moment within the observation period, and the pulsar flux at each frequency within the observation frequency band.

[0040] S2. Process the pulsar observation data obtained in S1 to obtain the pulsar pulse arrival time T.ni Where the subscript n represents the nth pulsar and the subscript i represents the i-th observation. In step S2, the pulsar observation data can be folded and de-dispersioned using the DSPSR software, and the data can be calibrated and the pulse arrival time T measured using the PSRCHIVE software. ni and its error Alternatively, the DFPSR software can be used directly to process the data and generate the pulsar arrival time T corresponding to each observed pulsar. ni and its error The data processing software used in step S2 includes any one or a combination of DFPSR, DSPSR, PSRCHIVE, TEMPO, TEMPO2, and PINT.

[0041] S3. The pulse arrival time T obtained in S2 ni Tracing back to International Atomic Time T′ ni In the process of tracing back to International Atomic Time (UTC), it is necessary to first use the clock difference files provided by the observatory (radio observatories usually provide corresponding clock difference files) to trace the atomic clock readings of the observatory to UTC. These clock difference files are obtained by comparing the atomic clock readings of the observatory with UTC using a satellite navigation system (such as GPS or BeiDou). After obtaining UTC, the time difference file between UTC and International Atomic Time provided by the International Earth Rotation and Reference Systems Service (IERS) can be used to trace UTC back to International Atomic Time T′. ni .

[0042] S4. Calculate the international atomic time T′ based on the known rotation laws of pulsars. ni The pulse arrival time T″ corresponding to the moment ni and pulse arrival time residual δT ni =T″ ni -T′ ni Using software that provides pulsar timing capabilities (such as DFPSR, TEMPO, TEMPO2, or PINT), the international atomic time T′ corresponding to the pulsar observation time is determined based on the pulsar rotation parameters. ni Calculate the corresponding pulse arrival time T″ ni and pulse arrival time residual δT ni =T″ ni -T′ ni The data processing software used in step S4 includes any one or a combination of DFPSR, DSPSR, PSRCHIVE, TEMPO, TEMPO2, and PINT.

[0043] S5. Analyze δT of each pulsar ni The power spectrum was used to determine the pulse arrival time residual δT for each pulsar. niThe power spectrum can be fitted with a second-order polynomial to the longest timescale δt corresponding to the red noise. n The specific implementation process is as follows:

[0044] S5.1. For each pulsar, use the formula Calculate the power spectrum of the pulse arrival time residual, where S n (t) represents the power spectrum of the pulsar pulse arrival time residual, where t is the independent variable of the power spectrum, and δT ni Let T′ be the pulse arrival time residual corresponding to the i-th observation of the n-th pulsar. ni The pulse arrival time T ni The corresponding International Atomic Time.

[0045] S5.2. Use in S represents the power-law spectral red noise component in the residual power spectrum of pulsar pulse arrival time. n1 (t)=C n This represents the white noise component in the power spectrum of the pulse arrival time residuals of pulsars. The corresponding parameter k for each pulsar is obtained by fitting the power spectrum of the pulse arrival time residuals. n α n With C n , where α n For spectral index, k n Power-law spectral red noise corresponding coefficients, C n This represents the intensity of white noise.

[0046] S5.3. For all I of the pulsar n Each group of consecutive observation segments in this observation and the corresponding pulse arrival time residual Perform a second-order polynomial fitting, the fitting function is Where a, b, and c are the parameters to be fitted to the polynomial.

[0047] S5.4. Examine the standard deviation of the fitted residuals With data segment length The changing relationship will satisfy the condition. The maximum δt is labeled as δt n The longest timescale corresponding to the red noise is fitted using a second-order polynomial.

[0048] Using the δt of this pulsar from the most recent observation forward n δT is obtained by processing all observation data within the time period. ni Second-order polynomial fitting was performed on the atomic clock readings at the observation station. The corresponding fitting residuals and second-order polynomial parameters are respectively labeled as follows: a n b n With c n , which serves as a set of parameters for predicting pulsar arrival times.

[0049] S6. Use the δt obtained from the analysis in step S5. n The pulsar observation time T is obtained by calculation with a second-order polynomial. ni The corresponding discrete pulsar time t p (T ni );

[0050] Calculate T ni The pulsar arrival time residual predicted by the second-order polynomial for each pulsar at time is: by As weight pairs Perform a weighted average to obtain the pulsar observation time T. ni The corresponding discrete pulsar time

[0051] S7. Using pulsar observations to determine the atomic clock reading T at the observation station ni The corresponding discrete pulsar time t p (T ni It can obtain the real-time pulsar time t corresponding to the atomic clock time reading T at any observation station at any given time. p (T). Consider δt n The minimum value δt n0 =min(δt) n ), for time T ni front δt n0 All pulsar observations within a given time correspond to discrete pulsar time t p (T ni Perform second-order polynomial fitting The optimal fitting result is the correspondence between the atomic clock reading T at the observation station and the real-time pulsar time t. p (T)=a0T 2 +b0T+c.

[0052] S8. Following the pulsar observations in S1, observe and record data from N pulsars using the same observation intervals and data recording methods. Process the data using the steps in S2 to obtain the pulse arrival times. Use the real-time pulsar time generated in S7 to replace International Atomic Time (IAT) to calculate the pulse arrival time residuals. From this step onwards, the atomic clock readings at the observation station are no longer traced back to IAT. Continue observing and recording data from the same pulsar group using the same method as in S1. Process the data using a similar method to S2 to obtain the pulse arrival times. The difference is that if IAT is needed during data processing, all relevant values ​​are replaced with real-time pulsar time, and the real-time pulsar time is used to replace IAT to calculate the pulse arrival time residuals.

[0053] S9. After each pulsar data update, repeat the processing procedure in step S5 using the most recent four years' data for that pulsar to obtain the second-order polynomial corresponding to the pulsar and the longest timescale corresponding to the fitted red noise. Specifically, after each observation to obtain new pulsar data, repeat the processing procedure in step S5 using the most recent four years' data for that pulsar to update the fitting residual of the second-order polynomial, the parameters of the second-order polynomial, and the longest timescale corresponding to the red noise that can be fitted by the second-order polynomial. a n b n c n With δt n ;

[0054] S10. Using the parameters obtained in S8 and S9, the real-time pulsar time is obtained using the methods in S6 and S7. Using the pulsar arrival time residual and polynomial parameters obtained in S8 and S9, the real-time pulsar time corresponding to the atomic clock reading at the observatory after each pulsar observation can be obtained using the methods in S6 and S7.

[0055] S11. After each new pulsar observation, execute S8-S10 again to obtain the real-time pulsar time corresponding to the atomic clock reading at the observatory after the latest observation.

[0056] In one specific embodiment, the present invention uses the pulse arrival time residual data of 20 pulsars generated by numerical simulation to conduct real-time pulsar time generation tests. The specific method is as follows:

[0057] The pulse arrival time residual can usually be considered as a superposition of red noise with a power-law spectrum and white noise with a flat spectrum. Due to fitting errors, it usually has a second-order polynomial residual with respect to the standard time velocity. Therefore, the pulse arrival time residual can be simulated by superimposing a random quadratic function with red noise (the intensity of which is the general intensity of the red noise used for timing millisecond pulsars in pulsar time studies) with a random spectral exponent of 2-4 and an intensity of 100-400 nanoseconds corresponding to a 10-year timescale, and white noise (the intensity of which is the general intensity of the white noise used for timing millisecond pulsars in pulsar time studies observed by the FAST telescope) and a random quadratic function. The pulse arrival time residual of 20 pulsars with an average interval of about 15 days over 27.4 years (each pulsar data length is 666, corresponding to 10,000 days) was generated as input data.

[0058] The first 97 data points for each star (corresponding to the data from the previous 4 years) were used as the first stage of observation data to analyze and obtain the white noise intensity of different pulsars, the longest time scale on which the red noise intensity can be fitted by a second-order polynomial, and the coefficients and standard deviation of the fitting residuals of the second-order polynomial corresponding to the last data segment within that time scale. All of the above data were recorded in a 20*6 array A.

[0059] Arrival time residuals of all pulses after the 98th pulse from the 20 pulsars are sorted by observation time and placed into an array of length 11380. An empty array of length 11380 is created (corresponding to the deviation between real-time pulsar time and International Atomic Time for all data starting from the 98th pulse). For each observation loop, the following operations are performed: using array A and the arrival time residuals of all pulses before this observation, and the difference between the discrete pulsar time and International Atomic Time before this observation, the difference between real-time pulsar time and International Atomic Time for the corresponding observation data point is calculated. After the loop is completed, the difference between real-time pulsar time and International Atomic Time of length 11380 is obtained, which represents the difference between real-time pulsar time and International Atomic Time corresponding to each pulsar observation. The calculated difference between real-time pulsar time and International Atomic Time starting from the 5th year is as follows. Figure 2 As shown, the difference between real-time pulsar time and International Atomic Time is less than 35 nanoseconds within a timescale of 23.4 years, proving that the method proposed in this invention is effective.

[0060] Furthermore, the present invention also provides a system for generating real-time pulsar time independent of the atomic time system using radio observations of multiple pulsars, for implementing the method of generating real-time pulsar time independent of the atomic time system according to the present invention using radio observations of multiple pulsars. The system includes an observation module and a calculation module. The observation module is used to observe N pulsars to obtain observation data, and the calculation module is used to generate real-time pulsar time based on the observation data and the local clock reading of the observation station.

[0061] This invention defines three types of pulsar times. In addition to the aforementioned "discrete pulsar time" and "real-time pulsar time", it also defines "non-real-time pulsar time". "Non-real-time pulsar time" is mainly aimed at the current pulsar time technology in the background art, which can only generate non-real-time pulsar times.

[0062] The advantages of this technology are:

[0063] This invention eliminates the influence of pulsar timing red noise through a polynomial fitting process within a short timescale, resulting in real-time pulsar times with higher frequency stability.

[0064] After the invention begins generating real-time pulsar times, it will operate independently of the atomic time system and generate real-time pulsar times.

[0065] This invention can obtain real-time pulsar times without complex data processing.

[0066] Any process or method described in the flowcharts of this invention or otherwise herein can be understood as representing a module, segment, or portion of code comprising one or more executable instructions for implementing a particular logical function or process, achievable on any computer-readable medium for use by an instruction execution system, apparatus, or device. The computer-readable medium can be any medium containing a program for storage, communication, propagation, or transmission for use by an execution system, apparatus, or device, including read-only memory, magnetic disks, or optical disks.

[0067] In the description of this specification, references to terms such as "embodiment," "example," etc., indicate that a specific feature, structure, material, or characteristic described in connection with that embodiment or example is included in at least one embodiment or example of the present invention. In this specification, the illustrative expressions of the above terms do not necessarily refer to the same embodiment or example. Furthermore, those skilled in the art can combine or combine the different embodiments or examples described in this specification and the features therein without causing contradiction.

[0068] While embodiments of the present invention have been shown and described above, it is understood that the above embodiments are exemplary and should not be construed as limiting the present invention. Those skilled in the art can make changes, modifications, substitutions, and alterations to the above embodiments within the scope of the present invention.

Claims

1. A real-time pulsar time generation method independent of atomic time systems, characterized in that, The method includes the following steps: S1. Select N radio pulsars with known rotation patterns, and use a radio telescope to successively observe and record the observation data of the N pulsars. Continue the observation in the first stage. The total number of observations of pulsars is denoted as N is greater than or equal to 10; S2. Process the obtained pulsar observation data to obtain the pulsar pulse arrival time. subscript Representing the Pulsar, subscript Representing the Second observation; S3. Obtain the pulse arrival time Tracing back to the International Atomic Time ; S4. Calculate International Atomic Time based on the known rotation laws of pulsars. Pulse arrival time corresponding to the time and pulse arrival time residual ; S5. Analyze each pulsar The power spectrum was used to determine the pulse arrival time residual for each pulsar. The longest timescale corresponding to the red noise can be fitted in the power spectrum using a second-order polynomial. ; S6. Using the analysis obtained in step S5 Pulsar observation times were obtained by calculation with second-order polynomials. The corresponding discrete pulsar time ; S7. Using pulsar observations to determine the time reading of the atomic clock at the observation station. Corresponding discrete pulsar time get The atomic clock reading at the observation station at any subsequent time Corresponding real-time pulsar time ; S8. After the pulsar observation in S1, observe N pulsars successively with the same observation interval and data recording method, record the observation data, and process the data using the steps in S2 to obtain the pulse arrival time. Use the real-time pulsar time generated in S7 to replace the international atomic time to calculate the pulse arrival time residual. S9. After each pulsar data update, repeat the processing in step S5 using the data from the most recent 4 years of the pulsar to obtain the second-order polynomial corresponding to the pulsar and the longest timescale corresponding to the fitted red noise. S10. Using the parameters obtained in S8 and S9, the real-time pulsar time is obtained using the methods in S6 and S7; S11. After each new pulsar observation, execute S8-S10 again to obtain the real-time pulsar time corresponding to the atomic clock reading at the observatory after the latest observation.

2. The real-time pulsar time generation method independent of atomic time systems according to claim 1, characterized in that, In step S1, the first phase lasts for 4 years; each observation of each pulsar lasts for no less than 15 minutes, and the interval between two consecutive observations of each pulsar is maintained between 10 and 20 days.

3. The real-time pulsar time generation method independent of atomic time systems according to claim 1, characterized in that, In step S1, the observation data includes the variation of radiation data of different frequencies of pulsar radiation over time and the observation time.

4. The real-time pulsar time generation method independent of atomic time systems according to claim 1, characterized in that, In step S2, the pulse arrival time obtained is based on the atomic clock reading at the observation station.

5. The real-time pulsar time generation method independent of atomic time systems according to claim 1, characterized in that, In step S3, during the process of tracing back to International Atomic Time, tracing the atomic clock readings of the observation station to International Atomic Time requires the use of clock difference files obtained through satellite navigation systems that are compared with Standard Coordinated Universal Time, as well as time difference files between different times provided by the International Earth Rotation and Reference Systems Service.

6. The real-time pulsar time generation method independent of atomic time systems according to claim 1, characterized in that, In step S4, the pulse arrival time residual is obtained. At the same time, the error of the pulse arrival time residual can be obtained. .

7. The real-time pulsar time generation method independent of atomic time systems according to claim 1, characterized in that, In step S5, the power spectrum of the pulsar pulse arrival time residual. The superposition of red noise with a power-law spectrum and white noise with a flat spectrum is used, and the residual power spectrum of the pulsar pulse arrival time is set to be equal to a power-law function. With a constant function The sum of these parameters is used to fit the power spectrum of the observed pulsar pulse arrival time residuals to obtain the parameters of the power-law function and the constant function. and ; in the same subscript Pulse arrival time residual sequence In, there exists Makes any sequence and , , , , , The correspondence is obtained using second-order polynomials. After fitting, the standard deviation of the corresponding fitting residuals All less than or equal to Those that meet the above conditions In the middle, take the largest one and denote it as The longest timescale corresponding to the red noise is fitted using a second-order polynomial. Represents all pulsars The first observation in the second observation A group of continuous observation segments.

8. The real-time pulsar time generation method independent of atomic time systems according to claim 7, characterized in that, In step S6, the information obtained in step S5 is used. Pulsar observation times were obtained by calculation with second-order polynomials. The corresponding discrete pulsar time :predict Pulse arrival time residual corresponding to time 1 ,by As weight pairs Perform a weighted average to obtain the discrete pulsar time. .

9. A real-time pulsar time generation system independent of atomic time systems, characterized in that, The system is used to implement the real-time pulsar time generation method independent of atomic time system according to any one of claims 1-8; the system includes an observation module and a calculation module, the observation module is used to observe N pulsars to obtain observation data, and the calculation module is used to generate real-time pulsar time based on the observation data and the local clock reading of the observation station.

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